Unconventional Stable Isotope Approaches and Systems

Isotope GeochemistryW, M. White Chapter 11UNCONVENTIONAL ISOTOPES AND APPROACHES11.1 INTRODUCTIONTraditional stable isotope geochemistry, the field developed by Harold Urey and his students, focusedon simple isotope ratios of light elements that can be analyzed in a gas source mass spectrometer:1 H/ 2 H, 13 C/ 12 C, 15 N/ 14 N, 18 O/ 16 O, and 34 S/ 32 S. Over the past decade or two, stable isotope geochemistryhas expanded in three important new directions.First, geochemists have begun to exploit the tendency of isotopes of pairs of elements, particularlycarbon and oxygen, to “clump” in thermodynamically preferred isotopologues. We introduced thetheoretical basis of this approach in Chapter 8. In this chapter, we explore some examples of the usesand applications of this approach.Second, by analyzing additional isotope ratios of oxygen and sulfur, specifically 17 O/ 16 O and 33 S/ 32 S,mass-independent fractionations were discovered in terrestrial materials in the past decade or so. Aswe found in Chapter 8, both equilibrium and kinetic effects should produce fractionations whose magnitudedepends on the relative mass difference between the isotopes of interest; this is known as massdependentfractionation. However, reactions induced by relatively high-energy photons in the atmospherecan produce fractionations in which the magnitude of fractionation is independent of the massdifference between isotopes. Studying these mass-independent fractionations have led to importantnew insights into Earth processes and evolution.Third, the list of elements of interest has greatly expanded, including both light elements such as Liand B, which we can expect will experience relatively large fractionations, but also heavier metals andgases such as Mg, Si, Cl, Ca, Fe, Cu, Zn, Se, Mo, Tl Hg, and U, which experience smaller, but nonethelesssignificant fractionations. A variety of techniques are used in analysis including thermal ionization(for example, B can be analyzed as the heavy ion CsBO + 2 ), gas source mass spectrometry (Cl), multi-Table 11.1. Values of Non-Conventional Stable Isotope RatiosElement Notation Ratio Standard Absolute RatioLithium δ 7 Li7 Li/ 6 Li NIST L-SVEC 12.1735Boronδ 11 B11 B/ 10 B NIST 951 4.0436Magnesium δ 26 Mg26 Mg/ 24 Mg DSM3 0.13979Silicon δ 30 Si30 Si/ 28 Si NBS28 (NIST-RM8546) 0.033532δ 29 Si29 Si/ 28 Si 0.050804Chlorine δ 37 Cl37 Cl/ 35 Cl seawater (SMOC) 0.31963NIST-SRM 975 0.31977Calcium δ 44/42 Ca44 Ca/ 42 Ca NIST SRM 915a 0.310163δ 44/40 Ca44 Ca/ 40 Ca 0.021518δ 43/42 Ca43 Ca/ 42 Ca 0.208655Ironδ 56 Fe56 Fe/ 54 Fe IRMM-14 15.698δ 57 Fe57 Fe/ 54 Fe 0.363255Copper δ 65 Cu65 Cu/ 63 Cu NIST 976 0.44562Zincδ 68 Zn68 Zn/ 64 Zn JMC3-0749L 0.37441δ 66 Zn68 Zn/ 64 Zn 0.56502Molybdenum δ 97/95 Mo97 Mo/ 95 Mo various* 0.5999δ 98/95 Mo98 Mo/ 95 Mo 1.5157*No interlaboratory standard has been agreed upon. Based on data listed in Coplen et al. (2002).327 1/9/13

Isotope GeochemistryW, M. White Chapter 11collector ICP-MS, and ion probe techniques. The theoretical principles are the same as we discussed inChapter 8: heavier isotopes will enter the phase with the stronger bond and the extent of fractionationdepends on temperature. The largest fractionations will occur where the element is partitioned betweenphases in which the element’s atomic environment is very different or its oxidation statechanges. Biologically mediated reactions produce some of the largest fractionations for these new elements,particularly Fe, Cu, and Zn, just as was the case for traditional elements C, N, and S. The list ofthese “non-traditional” stable isotopes is sufficiently long that we have space here only to “highlight”some of the more fascinating insights these studies have provided. More details on these elements canbe found the Volume 55 of Reviews in Mineralogy: Geochemistry of Non-Traditional Stable Isotopes (Johnsonet al., 2004). These non-traditional stable isotopes are summarized in Table 11.1.11.2 APPLICATIONS OF ISOTOPIC CLUMPINGWe introduced the theory behind isotopic “clumping” studies in Chapter 8. Here we’ll consider applicationsto geothermometry and paleoclimatology. A significant advantage of clumped isotope geothermometryis that, assuming equilibrium was achieved between a carbonate mineral and the waterfrom which it precipitated and no subsequent disturbance of the system, both paleotemperatures andthe isotopic composition of the water can be determined from analysis of the carbonate. This is becausethe ∆ 47 parameter (a measure of the abundance of the 13 C 18 O 16 O isotopologue relative to a purely stochasticdistribution we introduced in Chapter 8) is a function only of the equilibrium temperature for agiven mineral. Once the equilibrium temperature is known, then the δ 18 O and δ 13 C of the water can becalculated from the δ 18 O and δ 13 C of the carbonate (e.g., equation 10.1).We saw in Chapter 10 how oxygen and hydrogen isotope geothermometry has successful determinedthe cause of the Pleistocene “Ice Ages” and reconstructed climate variation through the Cenozoic.Qualitative proxies such as fossils and glacial sediments indicate that dramatic climate variations alsooccurred in the Mesozoic and, particularly, the Paleozoic: there is evidence of glaciation in the Carboniferousthat was as severe as the Pleistocene as well as evidence for perhaps less severe glaciation in theLate Ordovician, with intervening periods that appear to have been significantly warmer than the present.Such warmer temperatures would be consistent with much higher modeled atmospheric CO 2 concentrationsin the Paleozoic (such as shown in Figure 10.43). However, oxygen isotope geothermometrybased on carbonate fossils suggests that variations of tropical sea surface temperatures were relativelywas small over this time. Conventional isotope geothermometry, however, necessarily requires assumptionsabout the oxygen isotopic composition of seawater of the time. For the Pleistocene and eventhe Tertiary, the isotopic composition of seawater is readily constrained (as discussed in Chapter 10).This is not so easily done for periods earlier in Earth’s history. Veizer et al. (1999) argued, based onanalysis of marine carbonate fossils, that δ 18 O increased from a mean value of about -8‰ in the Cambrianto a present value close to 0‰. Muehlenbachs, however, has argued that seawater δ 18 O has beenbuffered by ridge-crest hydrothermal activity to values close to 0 throughout Earth’s history (Muehlenbachs,1976; Muehlenbachs and Furnas, 2003; Chapter 9).To address these issues, Came et al. (2007) analyzed carbon and oxygen isotopes of Silurian brachiopodsfrom Anticosti Island, Canada and Carboniferous (Pennsylvanian) molluscs from Oklahoma; bothof these localities were tropical at the time. Came et al applied clumped isotope geothermometry to determinethe temperatures of seawater in which they grew. Although all samples appeared to be wellpreserved based on various criteria, some proved to have been diagenically altered, yielding unreasonablyhigh temperatures and anomalous δ 13 C and δ 18 O seawater values. The remaining samplesyielded growth temperatures of 24.9±1.7 ˚C for the Carboniferous, and 34.9±0.4 ˚C for the Silurian. TheCarboniferous temperatures are similar to or slightly lower than those of modern tropical seas, whilethe Silurian temperatures are significantly warmer. The authors point out that these temperature differencesare consistent with models of atmospheric CO 2 during the Paleozoic: CO 2 was substantiallyhigher in the Silurian than in the both the Carboniferous and the present. Came et al. also calculated328 1/9/13

Isotope GeochemistryW, M. White Chapter 11δ 18 O SMOW of seawater for both times and obtained values of -1.2±0.1‰ and -1.6±0.5‰, values quite closeto the modern one (the present seawater δ 18 O SMOW is, of course, 0, but is ~ -1.5‰ if Antarctic and Greenlandice is included). The results suggest that the δ 18 O of seawater has been approximately constant, atleast through the Phanerozoic, and that the low values of δ 18 O observed for Paleozoic carbonates byVeizer et al. (1999) appear to reflect a combination of higher seawater temperatures and, predominately,diagenetic alteration of the carbonates.For the second example, we fast-forward several hundred million years to the Pliocene of East Africa,the time and place of the emergence of the genus Homo. Abundant hominid fossils and artifacts of Plio-Pleistocene age have been found in the Turkana Basin, part of the East African Rift in Kenya. This areapresently is among the hottest 1% of land on the planet with a mean annual temperature of almost30˚C. Much of the basin is occupied by a saline lake, Lake Turkana, and the surround land is quite arid.But what was the climate there like as our genus evolved from Australopithecine ancestors? Some paleoclimaticproxies derived from fossil pollen assemblages suggest that late Pliocene temperatures werecooler than present, while other proxies and models suggest an even warmer climate. To resolve this,Passey et al. (2010) applied clumped isotope geothermometry to paleosols of Pliocene and PleistoceneFigure 11.1. (a) ∆ 47 and calculated soil temperatures of paleosols from the Turkana Basin, Kenya.Dashing line shows the average modern soil temperature at a depth of 50 cm. (b) Measured δ 13 C PDBand calculated δ 18 O SMOW of Turkana Basin paleosols. Data from Passey et al. (2010).329 1/9/13

Isotope GeochemistryW, M. White Chapter 11age from the Turkana Basin. Before doing so, however, they demonstrated that temperatures calculatedfrom ∆ 47 in modern soil carbonates did in fact reflect the climate in which they formed. They foundgood agreement between calculated temperatures from soil carbonates and mean annual temperaturesin tropical regions, although in temperature latitudes (such as California), soil carbonate clumped isotopetemperatures correlated with mean warm season temperature rather than mean annual temperature.That’s not surprising since we expect soil carbonates to form only with evaporation exceeds precipitation,and in temperature latitudes that occurs in summer. Passey et al. (2010 also measured modernsoil temperatures at 50 cm depth in the Turkana Basin and found that they typically were 4˚ higherthan mean average air temperature.The results of this study are shown in Figure 11.1a. Calculated clumped isotope paleosol temperaturesrange from 28˚ to 41˚C and average 33˚C, quite similar to the average modern soil temperature of35˚C measured by Passey et al. There is no secular trend apparent over the period from 4 to 0.5 Ma.Calculated δ 18 O SMOW and measured δ 13 C PDB values are shown in Figure 11.1b. There is a hint of an increasein δ 13 C PDB through time, consistent with an increasing component of C 4 grasses in the flora. δ 18 Oappears constant through the Pliocene but steadily increased through the Pleistocene, consistent withthe results of an earlier study of Turkana Basin paleosols (Cerling et al., 1988). There are several possiblecauses of the increase in δ 18 O, including changes in basin hydrology and regional atmospheric andoceanic circulation. The interpretation consistent with other paleoclimatic indicators from the area isthat the Turkana Basin, while equally hot, was less arid in the Pliocene than at present. Regardless, theresults show that our genus originated in one of the hottest climates on the planet, which on the onehand may explain or preference for warm weather and on the other makes our adaption, in some cases,to extremely cold climates all the more remarkable.A final example addresses the question of whether or not dinosaurs were warm-blooded, a questionwhich has lingered for over 105 years. Reptiles are, of course, cold-blooded (ectotherms) and oftenspend the early hours of the day warming themselves in the Sun before becoming active. For the largestdinosaurs, the sauropods, the problem was less keeping warm than keeping cool. Because of theirenormous mass, which exceeded 9 tons in some cases, their internal temperatures might have exceeded40˚C if they could not efficiently shed metabolically generated internal heat. Eagle et al. (2010) analyzedthe carbonate component from tooth apatite, Ca 5 (PO 4 ,CO 3 ) 3 (OH,CO 3 ,F,Cl), in modern 5 animal species:elephant, rhino, crocodile, alligator, and sand shark, whose estimated body temperatures ranged from37˚ to 23.6˚. They found that ∆ 47 of the carbonate component released by phosphoric acid digestionshowed the same relationship to temperature as for inorganic calcite (Chapter 8). The teeth of 2 fossilmammoths also analyzed yielded temperatures of 38.4±1.8˚C, within error of the body temperatures ofmodern elephants. Tooth dentin of the mammoths, however, yielded lower temperatures, but both δ 18 Oand rare earth patterns of the phosphate component suggested the dentin has suffered diagenetic alteration.Eagle et al. (2011) then analyzed tooth enamel from Jurassic sauropods. Teeth from the TendaguruBeds of Tanzania of 3 Brachiosausus fossils yielded temperatures of 38.2±1˚C and 2 fossils of Diplodocinaeyielded temperatures of 33.6±4˚C. Three Camarasaurus teeth from the Morrison Formation inOklahoma yielded temperatures of 36.9±1˚C, while one from Howe Quarry in Wyoming yielded alower temperature of 32.4±2.4˚C. These temperatures are 5 to 12˚C higher than modern crocodiliansand, with the exception of the Howe Quarry tooth, within error of modern mammals. They are also 4to 7˚C lower than predicted for animals of this size if they did not somehow thermoregulate. Theyauthors note that this does not prove that dinosaurs were endotherms, but it does indicate that theypossessed “combination of physiological and behavioral adaptations and/or a slowing of metabolicrate prevented problems with overheating and avoided excessively high body temperatures.” In modernmammals, tooth enamel is produced only in youth. If this was also true of sauropods, it indicatesthat maintained high body temperatures during youth, consistent with observation of bone structurethat suggests high growth rates.330 1/9/13

Isotope GeochemistryW, M. White Chapter 1111.3 MASS INDEPENDENT ISOTOPE FRACTIONATIONS11.3.1 Mass-Independent Fractionation of Oxygen in the AtmosphereIn Chapters 5 and 8, we found that oxygen isotopes exhibit mass independent fractionations in meteoritesand in atmospheric ozone. Mass independent fractionations of oxygen isotopes also occur inother atmospheric species, as may be seen in Figure 11.2. Atmospheric nitrates show particularlystrong mass independent fractionation. Nitrate forms in the atmosphere in a variety of ways. Somemechanisms are homogeneous phase reactions (i.e., they result from reactions entirely in the gas phase)with ozone or the OH molecule. Others are heterogeneous phase reactions, involving both gaseous andliquid phases such as water droplets. Larger fractionation occurs occur in the heterogeneous reactionsthan the homogeneous ones. Consequently, there is a seasonal variation in the isotopic composition ofatmospheric nitrate, such that fractionation is greater in winter months. This is a direct consequence ofgreater cloudiness in winter (more water droplets), and hence greater contribution of heterogeneousphase reactions in winter. The nitrate, dissolved in water droplets as nitric acid, is washed out of theatmosphere by rain and into streams, soil, etc. The signature of mass independent isotope fractionationthen propagates through entire ecosystems, providing a tracer of nitrate for scientific studies.Atmospheric sulfur oxides also exhibit mass independent isotope fractionation. Sulfur makes its wayinto the atmosphere in a number of ways: volcanic emission of H 2 S and SO 2 , biomass burning (both anthropogenicand natural), and oxidation of dimethyl sulfide (C 2 H 6 S), which is emitted by marine plankton.Once in the atmosphere, the various forms of sulfur are oxidized to SO 3 and then to sulfate (SO 4 2- ).As with NO 2 oxidation, this last step may be either a homogeneous reaction in the gas phase, such as:SO 3 + H 2 O + M → H 2 SO 4where M is another gas phase molecule, or a heterogeneous reaction in which sulfate is produced in solution(in a water droplet) by reaction with H 2 O 2 or O 3 . Interestingly, only the heterogeneous phase re-Figure 11.2. Oxygen isotopic composition of atmospheric oxygen-bearing species. From Thiemens(2006).331 1/9/13

Isotope GeochemistryW, M. White Chapter 11Figure 11.3. ∆ 17 O in sulfates in ice from the Vostok ice core. Greater mass independent fractionationimplies a drier climate during glacial periods. Data from Alexander et al. (2002). From Thiemens(2006).actions result in mass independent fractionation, with the ozone oxidation pathway producing a muchlarger fractionation than the peroxide one. Once formed, the sulfate retains its mass independent fractionatedsignature on at least million year time scales (except under conditions of high acidity). This allowstracing of sulfur pathways through the atmosphere and biosphere on geologic time scales. For example,sulfate salts in the dry valleys of Antarctica were shown to be derived in part from atmosphericoxidation of marine dimethyl sulfide.Perhaps the most interesting application to come out of mass independent fractionation of sulfates isa measure of paleo-cloudiness. Again, as with the nitrates, mass independent fractionations are greatestwhen the oxidation occurs in solution. Consequently, more abundant droplets in the atmosphereresult in a greater average extent of mass dependent fractionation of sulfates. Turning that around,greater mass independent fractionation of oxygen in sulfates implies greater cloudiness. Figure 11.3shows that mass independent oxygen isotope fractionation in sulfates in Vostok ice follows the δDcurve. This is consistent with other evidence suggesting glacial period were drier, with fewer clouds.11.3.2 Mass Independent Sulfur Isotope Fractionation and the Rise of AtmosphericOxygenSulfur isotope fractionations in the modern Earth are usually mass dependent and δ 33 S and 36 S are relatedto variations in δ 34 S asδ 33 S = 0.515 x δ 34 S and δ 36 S = 1.90 x δ 34 SSome processes can produce mass independent fractionations. Let’s define the quantities ∆ 33 S and ∆ 36 Sas:∆ 33 S = δ 33 S - 0.515 × δ 34 S 11.1332 1/9/13

Isotope GeochemistryW, M. White Chapter 11and ∆ 36 S = δ 36 S – 1.90 × δ 34 S 11.2Mass independent fractionation of sulfur isotopes has been reported from sulfate aerosols from largevolcanic eruptions, such as the 1991 eruption of Pinatubo, but not for smaller eruptions (Savarino, et al.2003). The mechanism also appears to involve photolysis of SO 2 by ultraviolet light. Large plinianeruptions loft ash and aerosols into the stratosphere, whereas the products of smaller eruptions are confinedto the troposphere.In the modern Earth mass independent fractionation of sulfur is rare and appears to occur only in sulfurlofted into the stratosphere by the largest volcanic eruptions where it is exposed to ultraviolet light.However, Farquhar et al. (2000) found that many sulfides (primarily pyrite) in sediments and metasedimentsformed prior to 2500 Ma have positive ∆ 33 S and negative ∆ 36 S while hydrothermal sulfideores and sedimentary sulfates (mainly barite) have negative ∆ 33 S and positive ∆ 36 S (Figure 11.4). Duringthe Archean, ∆ 33 S, i.e., deviations from mass-dependent fractionation, of over 3‰ occurred. Farquhar etal. found smaller deviations, up to ½ ‰ in rocks from the period 2500-2000 Ma. They found no significantdeviations from mass dependent fractionation in rocks younger than 2000 Ma.This raises the obvious question of what process or processes operated during the Archean that couldproduce mass independent fractionation? Why is this process now rare? As mentioned in Chapter 8,mass independent isotope fractionation has been observed during laboratory photolysis of SO 2 and SOusing ultraviolet light. This, together with the observation that ozone and molecular oxygen absorb ultravioletradiation, provides a possible explanation. Modern volcanic eruptions loft vast quantities ofSO 2 into the atmosphere and Archean eruptions likely did as well. If the Archean atmosphere lackedO 2 and O 3 , ultraviolet radiation could penetrate deeply into it and photodissociate SO 2 . According toexperiments, these reactions produce sulfate with negative ∆ 33 S and elemental sulfur with positive ∆ 33 S.The sulfate would dissolve in rain and ultimately find its way into the oceans. Some of this would pre-Figure 11.4. ∆ 33 S in sulfur through time. During Stage 1 (prior to 2.45 Ga), extensive mass independentfractionation occurred as evidenced by ∆ 33 S up to 3.5‰, indicating the lack of atmosphericoxygen. During Stage 2 (2.45 to 2.0 Ga), limited amounts of atmospheric oxygen absorbedmost UV radiation and limited mass independent fractionation to

Isotope GeochemistryW, M. White Chapter 11cipitate as barite, BaSO 4 . Some sulfate would be reduced in hydrothermal systems and precipitate asmetal sulfides. Both these processes occur in modern oceans. The S would form particulate S 8 and alsobe swept out of the atmosphere by rain and ultimately incorporated into sediments, where it would reactto form sedimentary sulfides. The latter also requires an absence of O 2 in the atmosphere: as we discussedin the previous section, elemental S in the modern atmosphere is quickly oxidized to sulfate.Mass independent fractionation in Archean sulfur thus provides evidence that the early atmospherelacked free oxygen. This is entirely consistent with other evidence, such as the oxidation state of paleosolsand detrital minerals, that the atmosphere did not contain significant amounts of O 2 until the earlyProterozoic, about 2.4 billion years ago. Farquhar and Wing (2003), Kasting and Catling (2003), andCanfield (2005) provide excellent reviews on this topic.Mass independent fractionated of sulfur has also been found in sulfide inclusions in diamond, whichexhibit ∆ 33 S values up to +0.6‰ (Farquahar et al., 2002). The diamonds in question, from the Orapakimberlite in Botswana, are of the ‘eclogitic’ type, which also exhibit highly negative δ 13 C and highlyvariable δ 15 N, suggesting an ancestry of subducted sedimentary organic matter. Dating of silicate inclusionsin some ‘eclogitic’ diamonds give Archean ages. Thus the Archean atmospheric sulfur hadworked its way into the mantle. More recently, mass-independent fractionated sulfur has been reportedfrom late Archean volcanogenic massive sulfides (VMS) and komaiite-hosted NiS deposits (Bekker etal., 2009) – the latter indicating that atmospheric sulfur found its way into magmatic systems, mostlikely through assimilation of crust andearlier-formed VMS deposits. Mostrecently, Cabal et al. (2013) have reportedmass independent fractionations in sulfideinclusions in olivines of basaltic lavas fromMangaia, Cook Islands. These are shown inFigure 11.5 along with the compositions ofsulfide inclusions in diamonds reported byFarquahar et al. (2002). Mangaia, as we sawin Chapter X, has the most extreme of theSt. Helena or HIMU-type OIB Pb and Srisotopic signature. Again, there is noknown mechanism for producing massindependent fractionation of sulfur otherthan in the atmosphere, and that occurredalmost exclusively in the Archean. Thissulfur must thus represent sedimentarysulfur transported into the mantle throughsubduction and only returned to theEarth’s surface 2.5 Ga or more later. Itprovides dramatic confirmation thatmaterial of surfacial origin is indeed transporteddeep within the Earth and returnedto the surface through mantle plumes.Figure 11.5. Sulfur isotope composition of sulfide inclusionsin diamond (Farquahar et al., 2002) and olivinesfrom basaltic lavas of Mangaia, Cook Islands (Cabal, etal., 2013). Three of four of the Mangaia sulfides appearto form a mixing trend to an component with low δ 34 Sand low ∆ 33 S. A fourth Mangaia inclusion of secondaryorigin had ∆ 33 S ≈ 0. After Cabal et al. (2013).11.4 ISOTOPES OF IRON AND MOLYBDENUMAdditional insights into the oxygenation of the atmosphere and ocean have come from the isotopes ofiron and molybdenum, metals that never form gases under conditions prevailing on Earth. Both Fe andMo are transition metals that exist in several oxidation states. Both are bioessential elements. Ironplays a variety of rolls in life, from photosynthesis in plants to oxygen transport in animals. Molybde-334 1/9/13

Isotope GeochemistryW, M. White Chapter 11num is essential in bacterial nitrogen fixation (i.e., conversion of N 2 to NH 3 ; recall that only bacteria arecapable of nitrogen fixation) and is an important component of many key enzymes, both in bacterialand eukaryotes like you and I. In the modern ocean, these two elements behave very differently. Inmost environments at the surface of the Earth, iron is in the Fe 3+ state and is highly insoluble. This, andits rapid uptake by phytoplankton, keeps its concentration in the ocean quite low and variable, near 1 x10 -9 M, despite being the most abundant element in the Earth. The reduced form of iron, Fe 2+ is muchmore soluble. Molybdenum at the surface of the Earth is generally in the Mo 6+ state and forms thehighly soluble molybdate ion (MoO 4 2- ) in aqueous solution. Consequently, its concentration in theocean is about 1 x 10 -7 M and varies only in proportion to total dissolved solids (i.e., salinity). In reducingenvironments, Mo can be reduced to the IV form where it can form molybdenum sulfide ormolybdenum-iron sulfide phases.11.4.1 Fe Isotopes and the Great Oxidation EventFe has four stable isotopes: 54 Fe, 56 Fe, 57 Fe, and 58 Fe, whose abundances are 5.85%, 91.74%, 2.12%, and0.28%, respectively (Cousey et al., 2011). Most research has focused on the ratio of the two most abundantisotopes, 56 Fe/ 54 Fe, expressed as δ 56 Fe; some studies also report 57 Fe/ 54 Fe as δ 57 Fe and 57 Fe/ 56 Fe asδ 57/56 Fe. δ values are mostcommonly reported relative tothe IRMM-14 standard whoseisotopic composition is 56 Fe/ 54 Fe= 15.698, 57 Fe/ 54 Fe = 0.36325 and58 Fe/ 54 Fe = 0.04823, althoughsome workers use averageigneous rocks as the standard todefine δ 56 Fe (i.e., δ 56 Fe igneous rocks ≡0; e.g., Johnson et al., 2008). Herewe will discuss iron isotopesrelative to the IRMM standard,i.e., δ 56 Fe IRMM-14 . Since allvariations in iron isotopes observedto date fall along massdependentfractionation trends,we will consider only δ 56 Fe(where only δ 57 Fe values werereported, these have beenconverted to δ 56 Fe using δ 56 Fe =δ 57 Fe × 0.668; values reportedrelative to average igneous rockhave been converted using δ 56 Fe-IRMM-14 = δ 56 Fe igneous rocks + 0.014‰.)Variation of δ 56 Fe is shown inFigure 11.6. Igneous rocks showonly very limited variation.Ninety-four published analysesof peridotites whole rocks have amean δ 56 Fe IRMM-14 of 0.00‰, witha standard deviation of ±0.11‰.This value likely represents thecomposition of the bulk silicateFigure 11.6. Variation of δ 56 Fe in terrestrial materials and meteorites.335 1/9/13

Isotope GeochemistryW, M. White Chapter 11Earth. Larger variations occur in individual peridotite minerals. The average of 97 high precision analysesof oceanic basalts (mainly from Teng et al., in press) is slightly heavier, δ 56 Fe IRMM-14 = +0.11‰ with astandard deviation of 0.03‰. The difference between basalts and peridotites is consistent with a small(∆ 56 Fe ≈ -0.2‰) fractionation between olivine and silicate liquid during partial melting and fractionalcrystallization (e.g., Weyer et al., 2005; Teng et al., 2008) and with the observation that the most depletedperidotites typically have the lightest Fe (Williams et al., 2005). Granitoid igneous rocks areslightly heavier and more variable, δ 56 Fe = +0.16±0.07‰.Data summarized by Craddock and Dauphas (2011) show that carbonaceous and ordinary chondriteshave uniform δ 56 Fe values of -0.010±0.010‰ and -0.01 ±0.010‰, respectively; enstatite chondrites appearto be just slightly heavier, with δ 56 Fe of +0.020±0.0l0‰. On average, SNC meteorites (from Mars)have δ 56 Fe of -0.012±0.066‰ and HED meteorites (from 4 Vesta) have δ 56 Fe of 0.019±0.027‰, while lunarbasalts have a mean δ 56 Fe of +0.105±0.127‰ (0.073‰ if high-Ti basalts are excluded, which areslightly heavier) very similar to terrestrial ones (Weyer et al., 2005). Thus the three other planetary bodiesfrom which we have samples, the Moon, Vesta, and Mars, have Fe isotopic compositions that arenearly identical to each other and nearly indistinguishable from those of ordinary and carbonaceouschondrites. Iron meteorites have a mean and standard deviation δ 56 Fe of +0.050±0.101‰; magmatic ironmeteorites (those derived from asteroidal cores) have δ 56 Fe of +0.045±0.042‰ and are thus just slightlyheavier than chondrites (Poitrasson et al., 2005). Several experimental studies have found that the equilibriumfractionation between metal and silicate liquid at high temperature and pressure is quite small,with ∆ 56 Fe metal-slicate < 0.05‰ (Poitrasson et al., 2009; Hin et al., 2012) and cannot account for even thesmall (but statistically significant) difference in δ 56 Fe between iron meteorites and chondrites. The smalldifference in δ 56 Fe between peridotites (presumably representing bulk silicate Earth) and chondrites isalso statistically significant (although not above the 5% level) and could also not result from equilibriumfractionation during core formation. It is possible, however, that some as yet unrecognized formof kinetic fractionation could account for the difference; if so that could provide clues to the details ofthe core formation process.Looking at Figure 11.6, we see that most materials having δ 56 Fe significantly different than 0 havenegative δ 56 Fe. This includes high temperature hydrothermal fluids from mid-ocean ridges. While mostfluid samples have δ 56 Fe closer to 0, Fe-poor fluids can have δ 56 Fe as low as -0.8‰. The relationship toconcentration suggests the fractionation results from precipitation of Fe oxides and pyrites, with theisotopically lightest fluids being those from which the most Fe has precipitated (Johnson et al., 2008).The largest iron isotopic variation is observed in sediments and low-temperature fluids and is principallydue to the relatively large equilibrium fractionation (~+3‰) associated with oxidation of Fe 2+ toFe 3+ . However, Fe 3+ produced by oxidative weathering of igneous and high-grade metamorphic rocksis immobile, that is, isotopically heavy Fe 3+ remains bound in the solid phase in minerals such as magnetite,iron-bearing clays, and iron oxy-hydroxides. Thus weathering in an oxidative environment produceslittle net change is Fe isotopic composition. Weathering in a reducing environment, as wouldhave occurred in the early Archean, also produces little fractionation because there is no change in oxidationstate. In the transition from anoxic early Archean world to the modern oxic one significant poolsof both Fe 2+ and Fe 3+ would have existed, creating the potential for more significant variations in δ 56 Fe.The rise of atmospheric oxygen is, of course, a period of great significance in earth history and thereforeof great interest to earth scientists. We now consider the insights iron isotopes provide into this period.Johnson et al. (2008) argue that most of the fractionation evident in Figure 11.6 must be biologicallymediated, although coordination changes and abiotic oxidation and reduction may contribute smallfractionations. Two biological processes are important in reducing ferric iron in anoxic environments:dissimilatory iron reduction (DIR) and bacterial sulfate reduction (BSR). Both of these reactions occuronly in the absence of free oxygen. In DIR, iron is the electron receptor in the oxidation of organic carbon,which can be written as:4Fe(OH) 3 + CH 2 O + 8H + → 4Fe 2+ + CO 2 + 11H 2 O336 1/9/13

Isotope GeochemistryW, M. White Chapter 11In BSR, sulfur is the electron receptor in organic carbon oxidation:SO 4 2– + CH 2 O → 2HCO 3 – + H 2 SIron is then reduced by reaction with sulfide and precipitated as iron sulfide (e.g., pyrite). Of thesepathways, DIR produces the largest decrease in δ 56 Fe. In the Archean, ferric iron would have been rareor absent. However, many scientists believe that anoxygenic photosynthesis evolved before oxygenicphotosynthesis. Anoxygenic photosynthesis is performed today by green and purple bacteria who oxidizereduced sulfur in the course of reducing carbon. In the Archean, ferrous iron was likely a moreabundant reductant than sulfide and may have been used by early photosynthetic life in reactions suchas:4Fe 2+ + 7H 2 O + CO 2 → 4FeOOH + CH 2 O + 8H +The fractionation associated with this reaction is thought to be similar to abiotic iron oxidation. Photosynthesisthus would have provided a supply of ferric iron to feed an iron cycle operating in parallel tothe early carbon cycle.Figure 11.7 shows the variation of iron δ 56 Fe in various sedimentary materials over earth history. Aswe noted earlier, a variety of evidence, including sulfur isotope ratios, indicates that the atmospherelacked significant levels of O 2 until about 2.4 billion years ago. Between 2.4 and 2.2 Ga, a number ofchanges are observed: detrital pyrite and uraninite disappear from sediments, so-called red beds (sandstonesconsisting of quartz coated with hematite) appear, sulfates such as gypsum appear in evaporitesequences, and paleosols become Fe-rich, indicating soil Fe was in the immobile Fe 3+ form, all suggestingsignificant levels of atmospheric oxygen. Figure 11.7 shows that iron isotope ratios became distinctlymore variable around 2.8 billion years ago. A variety of works have argued that this indicatesthat significant pools of Fe 3+ were already available then, well ahead of the rise of atmospheric O 2 (e.g.,Johnson et al., 2008).Figure 11.7. Variation of 56 Fe in sediments through geologic time. Modified from Anbar and Roxel(2007) and Johnson et al., (2008) with additional data of Planavsky et al. (2012). Grey bar shows thetime of the rise of atmospheric oxygen, or the ‘Great Oxidation Event’ (GOE).337 1/9/13

Isotope GeochemistryW, M. White Chapter 11Even in the early Archean, elevated δ 56 Fe values are observed in banded iron formations. Banded ironformations (BIF’s) are marine sediments, typically consisting of layers of iron oxide (hematite or magnetite)alternating with layers of chert (in some cases, however, the iron is concentrated in clays or carbonates).They are thought to have formed when ferrous iron-rich deep ocean water upwelled to thesurface, the layering reflecting cyclic, perhaps annual, changes in upwelling. The ferrous iron was oxidizedto ferric iron and precipitated. Oxidation could have occurred through anoxygenic photosynthesis(Kappler et al., 2005) or through reaction with dissolved oxygen in the surface water produced byphotosynthesis. The later might be the best explanation for the smaller 3.7 to 3.8 billion year old BIFfound in Isua, Greenland, but oxygenic photosynthesis may have been involved in the massive BIF’s ofthe later Archean, such as the Hamersley deposit in Australia or the Mesoproterozic deposits near LakeSuperior in North America.The positive δ 56 Fe of BIF’s in the Archean and the first half of the Proterozoic is consistent with partialoxidation of a large pool of dissolved Fe 2+ , suggesting the deep oceans lacked dissolved oxygen. In thelate Archean and early Proterozoic, δ 56 Fe values in BIF’s become less variable, perhaps because oxidationof available Fe 2+ was more complete. The positive δ 56 Fe in BIF’s are complimented by negative δ 56 Fein black shales and pyrites, consistent with DIR of ferric iron. Both suggest that the surface waters ofthe ocean may have contained small by significant amounts of dissolved oxygen at this time. Furtherinsights into the oxygenation of the oceans and atmosphere come from Mo isotopes, which we explorein the following paragraphs.11.4.2 Mo Isotopes and Oxygenationof the OceansMo has seven stable isotopes: 92 Mo, 64 Mo,95 Mo, 96 Mo, 97 Mo, 98 Mo, and 100 Mo, whoseabundances are 14.77%, 9.27%, 15.90%,16.68%, 9.56%, 24.19%, 9.67% respectively(Cousey et al., 2011). All of these arerelatively abundant, but isobaric interferenceswith Zr make analysis of 92 Mo, 64 Mo,and 96 Mo difficult. Early studies reported the97 Mo/ 95 Mo ratio expressed as δ 97/95 Mo butmore recent studies generally reported the98 Mo/ 95 Mo ratio, expressed either as δ 98/95 Moor δ 98 Mo, since the variation in this ratio islarger. To date, there is no evidence of massindependent fractionation of molybdenumisotopes, so that δ 98/95 Mo ≈ 1.5 x δ 97/95 Mo. Nowidely accepted interlaboratory standardexists, although seawater, thought to havehomogenous Mo isotopic composition,provides a basis for comparison (seawaerδ 98/95 Mo = 2.45±0.11; Nakagawa et al., 2008).δ 98/95 Mo shows about 5‰ variation in terrestrialmaterials (Figure 11.8). Althoughsmall nucleosynthetic-related anomalies havebeen observed in meteorites (e.g., Burkhardtet al., 2011), their isotopic composition of isotherwise fairly uniform and similar to thatof terrestrial igneous rocks, with noFigure 11.8. Molybdenum isotopic variations in themodern Earth. Much of the range in seawater and igneousrocks may be the results of analytical error and interlaboratorybias. Modified from Anbar (2004).338 1/9/13

Isotope GeochemistryW, M. White Chapter 11systematic variations between meteorite classes (Becker and Walker, 2003). There appears to be littlevariation in igneous rocks, whose average δ 98/95 Mo is +0.07‰, suggesting little fractionation in hightemperatureprocesses. However, only 8 analyses of igneous rocks (2 granites and 6 Kamchatka basaltsanalyzed by Seibert et al., 2004) have been reported, so the igneous rock and bulk silicate Earth valuesare not well defined. Molybdenites (MoS 2 ) are somewhat more variable; the mean value of 60 analysesis +0.4‰ and Dahl et al. (2011) suggest this value, rather than the igneous rock mean, is representativeof the continental crust. Clastic sedimentary rocks have similar isotopic compositions and show similarlysmall variation. Rivers have positive δ 98/95 Mo with a flux-weighted average of about +0.7‰(Archer and Vance, 2008). This suggests some fractionation occurs during weathering, with light isotopespreferentially incorporated into secondary minerals or absorbed onto their surfaces. Analysis oflow temperature hydrothermal fluids at a single site suggests they have a similar δ 98/95 Mo of about+0.8‰ (McManus et al., 2002).The isotopic composition of seawater appears to be uniform throughout the open ocean, which is expectedgiven that the residence time of Mo in the ocean (~800 ka) is much longer than the mixing time.However, the δ 98/95 Mo of seawater is +2.3‰, about 1.5‰ higher than Mo delivered to the oceans byrivers. Clearly then, Mo isotope fractionation must be occurring in the marine system. Mn-Fe nodulesand crusts have δ 98/95 Mo of -0.5 to -1‰ and Barling et al. (2001) inferred that the low δ 98/95 Mo and highδ 98/95 Mo of seawater results from preferential adsorption of isotopically light Mo onto crusts. This fractionationhas subsequently been confirmed experimentally. Fractionation apparently also occursthrough preferential biological uptake of light Mo, but the fractionation is small (0.25‰). In part becauseonly a relatively small fraction of available Mo is biologically utilized, this fractionation probablyplays little role in producing the isotopic variations seen in Figure 11.8.Figure 11.9. Variation of δ 98/95 Mo in marine black shales and carbonates through geologic time. Becauseany fractionation is likely to result in lower δ 98/95 Mo in the sediment, it is the maximum valuesthat most likely represent seawater composition. The data suggest that limited amounts of O 2 werepresent in the oceans by the late Archean and that O 2 levels did not reach moderns levels until thePhanerozoic. Modified from Duan et al. (2010).339 1/9/13

Isotope GeochemistryW, M. White Chapter 11Mo in marine sediments deposited under euxinic conditions ‡ , such as the Black Sea or the CariacoBasin, has isotopic compositions close to that of seawater; i.e., the fractionation appears to be 0. Thismay at first seem surprising, since a fractionation associated with valence state change is expected.There are two reasons for this. First, under euxinic conditions, such as prevail in the modern Black Seabeneath 200 m or so, dissolved Mo is scavenged nearly completely, limiting the potential for isotopicfractionation. Furthermore, rather than being immediately reduced under such conditions, Mo is firsttransformed from oxymolybdate to oxythiomolybdate ions (MoO 4-x S 2- x ) by substituting sulfur atoms foroxygen atoms (Helz et al., 1999). Fractionations do occur between these species, but they tend to besmall. The oxythiomolybdate ion is very particle reactive and readily absorbed onto surfaces, particularlyof organic particles, and scavenged from seawater in that way. Only after incorporation intosediments is Mo reduced to Mo 4+ (Helz et al., 1999). In contrast, Mo in sediments deposited under oxygen-poor,but not euxinic, conditions have an average isotopic composition of δ 98/95 Mo ≈ +1.6‰(Brucker et al., 2009). In these environments, which are typical of some continental shelves, sedimentpore waters become reducing and sulfidic within the first few 10’s of cm of the surface; and Mo in thepore water precipitates as Mo-Fe sulfide. Pore waters are isotopically heavy (up to +3.5‰), and boththe data on pore waters and sediments suggest a moderate fractionation of about -0.7‰ (McManus etal., 2002). The precipitation results in a concentration gradient such that Mo concentrations in pore waterdecreases with depth. Consequently, Mo from seawater diffuses into the sediment and such sedimentthus represent a sink for Mo dissolved in seawater.In the modern ocean, where oxic conditions prevail and Mo is a conservative element with uniformisotopic composition. About 30-50% of seawater Mo is removed by adsorption on Mn-Fe nodules andcrusts under oxic conditions. A roughly similar amount is removed by sulfide precipitation in pore waterand a much smaller fraction, 5-15%, removed by precipitation under euxinic conditions (see problem11.1). Of these three removal mechanisms, only oxic adsorption involves a significant isotopicfractionation. Because light isotopes are preferentially absorbed, seawater is isotopically heavy. Attimes in the past, however, when anoxic or euxinic conditions prevailed, Mo should have had an isotopiccomposition close to that of rivers (δ 98/95 Mo ≈ +0.7‰). Consequently, Mo isotopes in ancientsediments should provide information on the oxidation state of ancient oceans (Anbar and Rouxel,2007).Because the isotopic composition of euxinic sediments appears to be identical to that of seawater, theMo isotopic composition of sediments deposited under euxinic conditions, such as black shales, can beused to trace the isotopic composition of seawater through time. Voegelin et al. (2009) showed that nonskeletalcarbonates also incorporate Mo with only small isotopic fractionation, thus carbonates are alsoused as paleo-oceanographic tracers. In both black shales and carbonates any fractionations will likelyresult in a lower δ 98/95 Mo in the sediment, thus it is the maximum δ 98/95 Mo that most likely representsthe seawater value. Figure 11.9 shows the variation of Mo isotope ratios in marine sediments – principallyorganic-rich shales and carbonates through geologic time. The Mesoarchean record is sparse, butδ 98/95 Mo in sediments deposited prior to 2.7 Ga are low, lower than the modern river average andwithin the range of molybdenites and close to igneous rock values. This suggests an absence of fractionationduring both weathering and deposition, which is consistent with an oxygen-free atmosphereand ocean. Beginning about 2.7 Ga, however, δ 98/95 Mo begins to rise and reaches values about 1.5‰ by2.5 Ga (e.g., Voegelin, et al., 2010). Czaja et al. (2012) found a negative correlation between δ 56 Fe andδ 98/95 Mo in carbonates and shales from the late Archean Transvaal Basin of South Africa (Figure 11.10).Based on a dispersion/reaction model modeling, they argue that the correlation results as dissolvedFe 2+ by photosynthetically produced O 2 is oxidized in the photic zone of the ocean. As a consequenceFe(OH) 3 precipitates with positive δ 56 Fe and adsorbs isotopically light Moo on its surfaces. The residual‡In the terminology of Anbar and Rouxel (2007), euxinic refers to conditions when water contains measurableamounts of H 2 S, while anoxic refers to conditions without O 2 but also without H 2 S.340 1/9/13

Isotope GeochemistryW, M. White Chapter 11dissolved Fe 2+ and Mo, which has negative δ 56 Fe and positive δ 98/95 Mo is incorporated into carbonates.According to their model, O 2 concentrations in photic zone of the basin reached about 12% of that of themodern ocean. However, they argue that the atmosphere at the time may well have been essentially O 2free, with concentrations near 10 -5 of present levels.Throughout the subsequent Proterozoic, δ 98/95 Mo remains below +1.4‰. These values are consistentwith the idea that while the Proterozoic atmosphere contained significant amounts of O 2 , perhaps 10%of present levels, much of the deep ocean remained anoxic or euxinic. For example, Kendall et al (2009)calculated that 30-70% of Mo was removed from the ocean in euxinic sedimentation around 1.1 billionyears ago (compared to 5 to 15% today) and Dahl et al. (2011) found that the seawater δ 98/95 Mo value ofabout +1‰ in the late Protererzoic (750 Ma) implies that euxinic bottom water covered 1 to 4% of theseafloor, a 20- to 80-fold increase over the modern ocean. Dahl et al. (2010) suggest that δ 98/95 Mo subsequentlyincreased in two steps – the first was around the Proterozoic-Phanerozoic boundary, which isalso the time of the first multi-cellular animals, when δ 98/95 Mo briefly increases from Proterozoic valuesof 1.1-1.2‰ to about 1.8‰ before decreasing to 1.4‰. Dahl et al. (2010) interpret this as an increase inatmospheric oxygen fromProterozoic levels of a few percent ofpresent values to 10-14% of presentvalues in the early Proterozoic. Asecond increase occurred sometimebetween the mid-Silurian and themid-Devonian when δ 98/95 Moincreased to about +2‰. This secondevent correlates with both the diversificationof vascular plants andthe expansion of large predatory fishand Dahl et al. (2010) interpret it asindicative of a rise in atmospheric O 2levels to more than 40% of thepresent value. Although the oceansappear to be well oxygenatedthrough most of the subsequentlyPhanerozoic, occasional anoxicevents occurred, such as the endPermian event and Toarcian event ofthe early Jurassic, resulting in briefexcursions to lower δ 98/95 Mo. Basedon the constant δ 98/95 Mo of Fe-Mncrusts, the seawater δ 98/95 Mo valueappears to have remained the sameas the modern value throughout theCenozoic (Siebert et al., 2003).11.5 ISOTOPES OF COPPER AND ZINCFigure 11.10. Correlated δ 98/95 Mo and δ 56 Fe in late Archeancarbonates from the Transvaal Basin. Modelling suggests thecorrelation results from oxidization of dissolved Fe 2+ in thephotic zone of the ocean, followed by precipitation ofFe(OH) 3 and adsorption of dissolved Mo. Residual Fe incorporatedin carbonate is isotopically light Fe while residualMo is isotopically heavy. After Czaja et al. (2012).Like Fe and Mo, Cu and Zn are transition metals and as such tend to form a greater variety of bondsthan the alkali and alkaline earth metals. Copper is significantly siderophile and much, and perhapsmost, of the Earth’s inventory is in its core, whereas Zn is not and most or all the Earth’s inventory is inthe mantle and crust. Both are, however, chalcophile and most ores of Zn and Cu consist of sulfides orsecondary minerals produced from sulfides. Both are somewhat volatile, Zn much more so that Cu. The50% nebular condensation temperature of Cu is 1037K, that of Zn is 726K, similar to that of Pb. In addi-341 1/9/13

Isotope GeochemistryW, M. White Chapter 11tion, Zn forms volatile complexes such as ZnCl 2 that partition into volcanic gas phases. Zn exists essentiallyin only one valence, 2+; copper exists mainly in cupric form (the 2+ valance state) in low temperature,oxidizing environments at the surface of the Earth and it is predominantly in the cuprous (+1 valencestate) form at high temperature and in reducing environments. More rarely, Cu occurs as the nativemetal (i.e., the 0 valence * ). On the whole oxidation and reduction does not play a major role in Cuand Zn isotope fractionation, in contrast to Fe and Mo. Copper and zinc are slightly to moderately incompatibleelements, meaning their concentrations are higher in the crust than in the mantle and theirconcentrations tend to increase during fractional crystallization of mafic magmas. Like Fe and Mo, bothCu and Zn are bio-utilized and the largest isotopic fractionations occur as a consequence of biologicalprocesses.11.5.1 Cu IsotopesFormer Saudi oil minister Sheik Ahmed ZakiYamani once said, “The Stone Age didn't end for lackof stone”. It ended instead when people learned tosmelt copper and work it into tools and weapons. Inarcheological chronology, the Bronze Age succeededthe Copper Age when people found they could makestronger tools by alloying the copper with tin. In adifferent sense, the age of copper continues —because of its high conductivity and stability as ametal, we make very extensive use of it for wiringand piping. Copper remains the third most producedmetal (over 15,000 tons per year), following iron andaluminum. Perhaps no material has played as large arole of such a length of time in human civilization ascopper.Copper has two isotopes, 63 Cu and 65 Cu with abundancesof 69.15% and 30.85%, respectively (Cousey etal., 2009). Data are reported as δ 65 Cu relative to theNIST SRM976 † standard, whose 65 Ce/ 63 Cu ratio islisted in Table 11.1. Copper isotope variations inmeteorites and terrestrial materials is summarized inFigure 11.11. Cu isotope ratios vary significantly inmeteorites. Among chondrites, δ 65 Cu varies betweenclasses; among carbonaceous chondrites, δ 65 Cu decreaseswith increasing petrologic grade from -0.09%for CI1 to -1.45‰ for CV3. δ 65 Cu in ordinary chondritesshows a smaller range, -0.5‰ to -0.1‰ andFigure 11.11. Cu isotope ratios in terrestrial,lunar, and meteoritic materials.increases in order H, L, LL. Luck et al. (2003) found that δ 65 Cu correlated with oxygen isotope ratios andwith Ni/Cu ratios; Moynier et al (2007) showed that δ 65 Cu also correlated negatively with Ni and Znisotopic compositions. Luck et al. (2003) and Moynier et al (2007) et al interpret these variations as resultingfrom fractionations between silicate, metal, sulfide, and gas phases in the solar nebula followed* Native copper was first mined and exploited by primitive societies lacking smelting technology. One example is theKeweenaw native copper of Michigan, exploited by Native Americans of the region as their sole source of metal fortools and ornamental objects.† NIST stands for the U.S. National Institute of Standards and Technology and was formerly known as the NationalBureau of Standards, hence NBS is sometimes seen in place of NIST. SRM stands for standard reference material.342 1/9/13

Isotope GeochemistryW, M. White Chapter 11by sorting of these components and subsequent mixing in parent bodies. Even larger variations are observedin iron meteorites, which range from δ 65 Cu = -9.23‰ to δ 65 Cu =+1‰, although most fall within anarrower range of -2.5‰ to +0.25‰ (Williams and Archer, 2011; Bishop et al., 2012). These variationsresult from a number of factors including metal-silicate fractionation during segregation (∆ 65 Cu met.-sil. ≈-0.5‰), fractionation between solid and liquid metal phases, and fractionation between metal and sulfidephases (∆ 65 Cu met.-sulf. ≈ +0.64‰). However, the observed variations greatly exceed those expectedfrom equilibrium fractionations alone. Williams and Archer suggested they reflect kinetic effects duringexsolution of sulfide from the metal phases, including more rapid diffusion of the lighter Cu isotope,63 Cu. Lunar basalts have δ 65 Cu = +0.5‰, heavier than the silicate Earth, which Herzog et al. (2009) attributedto igneous fractionation.The very few data that have been published on ultramafic and basaltic rocks (e.g., Ben Othman et al.,2006) suggest that the δ 65 Cu of the bulk silicate Earth is in the range of 0-0.1‰. Li et al. (2009) found thatδ 65 Cu in most granites from the Lachlan Fold Belt of Australia varied between -0.15‰ to +0.21‰, andthat mean values for S- and I-type granites were indistinguishable at around 0‰. Two granites hadheavier isotopic compositions (up to +1.5‰) and two had significantly lighter compositions (down to-0.45‰), which Li et al. interpreted as a consequence of possible hydrothermal and secondary alteration.Thus in igneous silicate rocks, δ 65 Cu is nearly constant at 0±0.2‰ implying copper isotope fractionationsamong silicate minerals and melts are quite limited. Sediments and marine sedimentary particlestend to have slightly heavier isotopic compositions: δ 65 Cu = +0.08 to +0.35‰ (Maréchal et al.,1999).Not surprisingly, greater fractionations are observed when phases other than silicates are involved.Ehrlich et al. (2004) found that the fractionation during experimental precipitation of covellite (CuS)from copper sulfate solution varied with temperature as:∆Cuaq2+ −CuS(‰) =0.26 ± 0.02 ×106T 2 + 0.08 ± 0.25 11.3This reaction involves both precipitation and reduction (from Cu 2+ to Cu 1+ ) and results in the reducedprecipitate being isotopically lighter than the solution. However, the temperature range of their experimentswas small (10-40˚C). Pekala et al. (2011) reacted Cu 2+ solutions with pyrite and pyrrhotite attemperatures from 40 to 200˚C. Subsequent microscopic investigation showed the pyrite and pyrrhotitebeing replaced by covellite, chalcocite (Cu 2 S), and bornite (Cu 5 FeS 4 ), At temperatures up to 150˚C, theobserved fractionation followed that predicted by equation 11.3, but was greater than predicted (about2.5‰) at 200˚C. Pekala et al. argued that reduction was the key step controlling the isotopic fractionation.Fernandez,and Borrok (2009) reacted pyrite, chalcopyrite and sphalerite (ZnS) with acidic, oxidizedsolutions and found that the leached Cu was up to 2‰ heavier than that in the sulfide minerals.Thus during both dissolution and precipitation, copper sulfides are isotopically lighter than Cu 2+ in solution.Seo et al. (2007) carried out theoretical quantum mechanical calculations of fractionation factorsand found that fractionation between sulfide and chloride species in hydrothermal fluids, such as(CuCl 2 ) – and (Cu(HS) 2 ) – should be quite small. Larger fractionations appear possible if high temperaturevapor phase species such as Cu 3 Cl 3 or (CuCl 2 ) 2- were involved.As we noted, most copper ores are sulfides. Two of the main types of copper ore deposits, volcanogenicmassive sulfides and porphyry coppers, form by precipitation of sulfides from hydrothermal solution(seawater is the primary water source in the former, magmatic water in the latter). Most primarycopper sulfides minerals, such as chalcopyrite (CuFeS 2 ) and cubanite (CuFe 2 S 3 ), in these types of depositshave δ 65 Cu in a relatively narrow range 0±0.5‰, similar to igneous rocks and the bulk silicate Earth(Rouxel et al., 2004; Larson et al., 2003; Markl et al., 2006; Mathur et al., 2009). Since the copper in thesedeposits is derived from igneous rocks or magmas, this implies that the fractionations involved in theirformation are generally small. Native copper has isotopic compositions within this same range (Larsonet al., 2003). Rouxel et al. (2004) found that primary chalcopyrite and cubanite in mid-ocean ridge active343 1/9/13

Isotope GeochemistryW, M. White Chapter 11hydrothermal chimneys defined a wider range of -0.43 to +3.62‰. Chalcopyrite from massive sulfidedeposits and inactive vents is consistently depleted in 65 Cu relative to chalcopyrite in active vents (consistentwith the experimental studies mentioned above). Secondary minerals found at inactive ventsand in massive sulfide piles, which included atacamite (Cu 2 Cl(OH) 3 ) and bornite showed more variablecompositions (-2‰ to +4.7‰). Rouxel et al. argued that the relatively wide range of δ 65 Cu in primarysulfides resulted from secondary minerals being redissolved by hydrothermal fluids as the systemsevolved and the copper reprecipitated as primary sulfides. Thus, they reasoned, the oxidation of primarysulfides was the major cause of copper isotope fractionation in these systems.A much wider variation in δ 65 Cu, -17 to +10‰, is observed in secondary minerals (Mathur et al.,2009) that typically develop during weathering of sulfides in the near-surface. Mathur et al. (2009)found that Cu in the enriched supergene § zones is typically 0.4 to 5‰ heavier than primary ore deposit(the hypogene). Markl et al. (2006) found that relict primary chalcopyrite were typically isotopicallydepleted with δ 65 Cu down to -3‰; secondary cuprous minerals such as cuprite (Cu 2 O) were isotopicallyheavy (δ 65 Cu: +0.4 to 1.65‰) and secondary cupric mineral such as malachites (CuCO 3 (OH) 2 ) werealso usually isotopically heavy, but showed a wider range than cuprous minerals) (δ 65 Cu: -1.5 to+2.4‰).Sediment-hosted stratiform copper deposits are another important class of copper ore deposits. Theseform when relatively low temperature fluids (≤120˚C) dissolve copper and other metals from rocks thenprecipitate them within existing sedimentary formations. The Kuipferschiefer, a Permian organic- andcarbonate-rich shale (a bituminous marl) that extends over much of northern Europe is a classic example.Mildly oxidizing fluids leached Cu and other metals including Zn, Pb, and Ag from the underlyingred sandstones, carrying them into the overlying shale. Reaction with organic matter in the shale reducedthe fluids, which resulted in precipitation of the metals as sulfides. This mineralization likely occurredwhen rifting associated with the opening of the Tethys Ocean resulted in higher heat flow. δ 65 Cuin the principal copper minerals, which include bornite, chalcolite, digenite (C 9 S 5 ), and covellite, rangefrom about -2.7 to 0‰, but most fall within the narrow range of -0.4±0.36‰ (Asael et al., 2009). In asimilar stratiform copper deposit developed in Cambrian sediments of the Timna Valley, Israel, coppersulfides have much lighter isotopic compositions -2.00±0.4‰. Asael et al. (2009) explained the differencein terms of temperature, pH, and oxidation state of the fluids. In the Timna valley, the depositformed under mildly oxidizing conditions (E H values of 0.5 to 0.6), low temperature and mildly acidic(pH

Isotope GeochemistryW, M. White Chapter 11+0.09‰, which is about a per mil lighter than seawater, and one sample of human blood had δ 65 Cu of+0.3‰ (Maréchal et al., 1999).δ 65 Cu in rivers is isotopically heavy compared to silicate rocks, varying from +0.02 to +1.45‰, with adischarge-weighted average of +0.68‰. In comparison, riverine particulate matter is isotopically light(δ 65 Cu: -0.24 to -1.02‰) (Vance et al, 2008). Seawater has somewhat variable isotopic composition(δ 65 Cu: +0.9 to -1.5‰), but the variation is not systematic with depth, even though Cu concentrationstypically show surface water depletion and deep-water enrichment (Bermin et al., 2006; Vance et al.,2008). Vance et al. (2008) suggested that adsorption on particle surfaces controls the Cu isotopic compositionof rivers and seawater, with 63 Cu preferentially adsorbed on particle surfaces. This would seemrequire the opposite fractionation as that observed by Pokrovsky et al. (2008), who observed preferentialadsorption of 65 Cu. The apparent discrepancy is likely due to Pokrovsky’s experiments being carriedout with pure water, whereas seawater and river water contain abundant organic ligands thatcomplex most of the dissolved Cu. As we learned in a previous Chapter, the heavy isotope goes preferentiallyinto the strongest bond. In pure water, where dissolved copper can form only weak aquocomplexeswith water molecules, surface complexes are the stronger bond; in natural waters, bondswith dissolved organic ligands are stronger than surface complexes.11.5.2 Zn IsotopesZinc has five isotopes: 64 Zn (48.27%), 66 Zn (27.98%), 67 Zn (4.10%), 68 Zn (19.02%), and 70 Zn (0.63%)(Clousey et al., 2011). The 66 Zn/ 64 Zn and 68 Zn/ 64 Zn are of most interest and are reported as δ 66 Zn andδ 68 Zn. Early results were reported relative to a solution made from Johnson-Matthey Company (JMC)metal stock by workers at ENS Lyon. The supply of this standard has been exhausted, but despite this,most data continue to be reported relative to the JMC-0749 standard, so all values mentioned here arerelative to that standard, i.e., δ 66 Zn JMC . Some recent results have been reported relative to the Institutefor Reference Materials and Measurements standard IRMM-3702, whose isotopic composition is66 Zn/ 64 Zn = 0.56397±30, 67 Zn/ 64 Zn = 0.08217±4, 68 Zn/ 64 Zn = 0.37519±35, and 70 Zn/ 64 Zn = 0.01242±2), andthis may become the future convention. Data reported relative to the IRMM standard can be convertedas δ 66 Zn JMC = δ 66 Zn IRMM-3702 + 0.3‰. Zn isotopic variations reported to date are mass dependent (i.e.,δ 66 Zn, δ 67 Zn and δ 68 Zn are correlated) so we will focus only on δ 66 Zn.Data on terrestrial igneous rocks is limited; basalts range from δ 66 Zn JMC = +0.17 to +0.48‰, with anaverage of +0.31‰ (Ben Othman et al., 2006; Herzog et al., 2009; Telus et al., 2012; Paniello et al., 2012).The standard deviation is 0.08‰, which is comparable to analytical precision and suggests igneousfractionation of Zn isotopes is quite small. The value of δ 66 Zn JMC = +0.31±0.08‰ thus presumably representsthe composition of the bulk silicate Earth. Granitoid rocks have a similar range and average δ 66 Zn= +0.26‰ with no apparent difference between A, I, and S-type granites; pegmatites, however, areabout +4‰ isotopically heavier than granites, ranging from δ 66 Zn +0.53 to +0.88‰ (Telus et al., 2012).This likely results from preferential fractionation of heavy Zn isotopes into the hydrous fluids involvedin pegmatite formation (Telus et al., 2012), suggesting in turn that Zn is more strongly bound in thesefluids, probably primarily to chloride complexes, than it is to complexes in silicate magmas. The rangeof δ 66 Zn in most siliciclastic sediments overlaps that of igneous ones (Maréchal et al., 1999; 2000),suggesting there is little Zn isotope fractionation in weathering.Zinc in carbonaceous chondrites is slightly isotopically heavy, with δ 66 Zn JMC varying from +0.16 to+0.52‰ and averaging about 0.37‰. δ 66 Zn increases in the order CO-CV, CM, CI and correlates withchemical parameters suggesting the variation results from mixing between isotopically heavy and lightcomponents in the solar nebula (Luck et al., 2005). Ordinary chondrites are more variable, with δ 66 Zn JMCranging from -1.3 to +0.76‰, and averaging +0.1‰, similar to the bulk silicate Earth value. Zinc in EHenstatite chondrites is fairly uniform and similar to the silicate Earth, with δ 66 Zn JMC ranging from +0.15to +0.31‰; δ 66 Zn JMC is more variable and heavier in the EL group, ranging from 0.01 to 0.63‰ in EL3chondrites and from 2.26 to 7.35‰ in the EH6 group (Moynier et al., 2011). The EL chondrites tend to345 1/9/13

Isotope GeochemistryW, M. White Chapter 11be volatile element-depleted; the heavy Zn isotopic compositions suggest this depletion resulted fromevaporation, particularly in the EL6 group. HED achondrites (meteorites from Vesta) tend to be slightlyisotopically heavy compared to Earth (Paniello et al., 2009). Aubrites, reduced achondrites related toenstatite chondrites, have isotopically light Zn (δ 66 Zn JMC = -7.08 to -0.37‰. These very light compositionssuggest their zinc is derived from condensation from a vapor (Moynier et al., 2011). In irons, δ 68 Znvaries from -0.6 to +3.7‰. δ 66 Zn JMC correlates positively with δ 65 Cu in IIIA irons, probably as a result offractional crystallization of metal, silicate, and sulfide from a metal-rich magma. The widest range isseen in the IAB-IIICD group (thought to represent impact melts rather than asteroid cores) and probablyreflects complex interaction between the metallic liquid and the asteroid regolith (Luck et al., 2005).δ 66 Zn JMC in SNC (Martian) meteorites average +0.25‰±0.05, but the range, +0.13 to +0.35‰, completelyoverlaps that of terrestrial basalts, suggesting the Earth and Mars have similar Zn isotopic compositions(Paniello et al. 2012).Most lunar basalts are isotopically heavy and fall in the range of +0.46 to +1.9‰, averaging+1.43±0.32‰ with no apparent difference between high- and low-Ti lunar basalts. Pyroclastic beads aswell as two basalts are isotopically much lighter with δ 66 Zn JMC as low as -5.4‰ (Herzog et al., 2009; Panielloet al., 2012). The light isotopic compositions in pyroclastic beads and in some basalts likely representscondensation of isotopically light Zn from volcanic gases emitted during eruption. Partitioning ofZn into a vapor phase (probably as ZnCl 2 ) is consistent with the observation of strong Zn enrichment infumarole gases in terrestrial volcanoes (e.g., Symonds et al., 1987). Heavier values that occur in regolithand soil samples most likely result from sputtering and impact effects (Paniello et al., 2012). The distinctlyheavy isotopic composition of lunar zinc is best explained by evaporative loss of Zn during theMoon’s formation. Zinc, as we noted earlier, is volatile and is depleted in lunar basalts by 1 to 2 ordersof magnitude compared to terrestrial ones. Paniello (2012) found that the Moon’s zinc concentrationand isotopic composition can be explained if roughly 80-90% of the zinc was lost by evaporation with avapor/melt fractionation factor of α = 0.999. Lunar zinc isotope ratios thus support the giant impactmodel of the Moon’s formation.Some of the largest variation in δ 66 Zn occurs in sulfide minerals, which range from -0.43 to +1.33‰.John et al. (2008) found that 66 Zn in ridge crest hydrothermal fluids from a variety of sites in the Pacificand Atlantic ranged from +0.0 to +1.04‰, with isotopic composition correlating with temperature.High temperature (>350˚C) vent fluids had 66 Zn close to the basalt value (~0.3‰), while lower temperature(

Isotope GeochemistryW, M. White Chapter 11al. (2010). In systems involving water, therefore, speciation may introduce significant Zn isotope fractionations.Data on zinc isotopes in seawater is very limited and the Zn isotopic budget of seawater has yet to beworked out. δ 66 Zn ≈ +0.3‰ in a single sample of English Channel water, while in the upper 400 m ofNorth Pacific seawater, δ 66 Zn varying from -0.15 to +0.15‰ and correlating negatively with δ 65 Cu(Bermin et al., 2006). Although Zn concentrations are strongly depleted in surface water due to biologicaluptake, that study found no apparent correlation between δ 66 Zn and Zn concentration. Zn in eightdeep water samples from the Pacific and Indian Oceans appears to be slightly heavy compared to surfacewater and somewhat more isotopically uniform, with δ 66 Zn varying from +0.22‰ to +0.64‰ andaveraging δ 66 Zn = 0.45±0.14‰ (Bermin, 2006). Manganese nodules have δ 66 Zn that range from +0.53‰to +1.16‰ and average 0.90‰ (Maréchal et al., 2000). Thus there is an apparent positive fractionationof Zn isotopes in Mn nodule formation. The. John et al. (2008) estimate that the riverine and atmosphericinputs to seawater are relatively light 66 Zn ≈ 0.1 to 0.3‰; however, the principal source of Zn inseawater is hydrothermal fluids, which, as we found above, are isotopically variable, although perhapssomewhat heavier than the riverine source on average.Pichat et al., (2003) found that δ 66 Zn in sediments from ODP core 849 from the eastern equatorial Pacific,whose age ranged from 3 ka to 174ka, showed a general decrease with time, varying from +0.31 to+1.34‰. Superimposed on this decrease was a weak periodic variation with periodicities of 35.3 and21.2 ka. The material in the core was primarily biogenic: carbonate tests of cocolithophorids and foraminifera(and indeed, the analysis was restricted to the carbonate fraction of the sediment). The 21.2 kaperiodicity corresponds closely to the mean periodicity of the precession periodicity of the Milankovitchvariations (Chapter 10). Pichat et al thus interpreted these variations as climatic effects ofoceanic circulation (specifically equatorial upwelling) and biological productivity.Zinc is a remarkably important element in biology. It is the second most abundant transition metal,following iron, in organisms. It is found in all classes of enzymes as well as in transcription factors (proteinsthat bind to DNA sequences, effectively turning genes on and off). It is important in protein synthesisand membrane activity, conversion of CO 2 to bicarbonate ion and visa versa (in both plants andanimals), brain activity, leaf formation, digestion, and so on. Nevertheless data on Zn isotope fractionationin organisms is fairly limited at present (this will undoubtedly change in the future). In hydroponic‡ growth experiments with tomatoes, lettuce, and rice, Weiss et al. (2005) found that roots of theseplants preferentially took up isotopically heavy Zn from the growing solutions and that the shoots ofthe plants were isotopically light compared to the roots (by up to 0.5‰). Simple growth experiments ofMoynier et al. (2009) with lentils (beans) and bamboo confirmed the preferential transport of isotopicallylight Zn up the plant and into the leaves – suggesting the process is at least partially controlled bydiffusion. Fractionations observed in bamboo were up to 1‰. John et al. (2007) found that experimentallygrown marine diatoms preferentially took up isotopically light Zn and that the fractionation dependedon Zn concentrations. At low concentrations, the fractionation was about -0.2‰ but at higherconcentrations it was -0.8‰. The difference likely reflects two biochemical pathways being used totransport Zn into cell interiors: a high-affinity mechanism associated with a small isotopic fractionationpredominates at low concentrations but becomes saturated at higher concentrations, where the lowaffinitymechanism becomes dominant. In contrast, Andersen et al., (2011) found that Zn in cleaned diatomstests from sediment core tops from the Southern Ocean was isotopically heavy, with δ 66 Zn rangingfrom +0.7‰ to +1.5‰. δ 66 Zn correlated negatively with Zn concentrations in the tests and biogenicsilica accumulation rates in the sediment. Assuming that Zn concentrations in the tests correlates withZn concentrations in surface seawater in which the diatoms grew, this suggests surface seawater becomesisotopically heavier as it becomes progressively Zn-depleted by biological uptake. Because autotrophssuch as plants and diatoms preferentially take up Zn 2+ rather than organically complexed Zn,‡ Hydroponics is a method of growing plants from a solution without soil.347 1/9/13

Isotope GeochemistryW, M. White Chapter 11Zn, and because there is isotopic fractionation between species in solution, the degree to which fractionationsin biological systems reflect fractionations between dissolved Zn species rather than biochemicalprocesses will require further study. Zn isotope ratios in animals is remarkably variable, from-0.4 to 0.8‰; human blood appears to be more uniform and isotopically heavy (δ 66 Zn +0.3 to +0.4‰)(Cloquet et al., 2008; Marèchal et al., 1999).11.6 ISOTOPES OF BORON AND LITHIUMAlthough there are a few earlier works in the literature, there was little interest in the isotopic compositionof boron and lithium until about 25 years ago. This are perhaps several reasons for this: becauseboth elements have low abundances in the Earth, they have only one valance state in nature, neither Bnor Li form gaseous species that can be analyzed in the gas-source mass spectrometers conventionallyused for analysis of other stable isotopes, and the fractionation produced in thermal ionization massspectrometers, would exceed the natural ones. Since the development of new analytical techniques thatovercame this latter problem in the 1980’s, the fields of boron and lithium isotope geochemistry havedeveloped rapidly.Though both lithium and boron can occur as stoichiometric components of minerals, these mineralshave limited occurrence, and these elements generally substitute for other elements in silicates. Boronis relatively abundant in seawater, with a concentration of 4.5 ppm. Lithium is somewhat less abundant,with a concentration of 0.17 ppm. Both are “conservative” species in seawater, which is to saythey are always present in a constant ratio to salinity. In silicate rocks, the concentration of boronranges from a few tenths of a ppm or less in fresh basalts and peridotites to several tens of ppm inclays. Lithium concentrations in these materials typically range from a few ppm to a few tens of ppm.Boron has two isotopes: 10 B and 11 B whose abundances are 19.9% and 80.1%, respectively (Coursey etal., 2011). The 11 B/ 10 B is reported as per mil variations, δ 11 B, from the NIST SRM 951 standard. Li alsohas two isotopes: 6 Li and 7 Li whose abundances are 7.59% and 92.41%, respectively (Coursey et al.,2011). The 7 Li/ 6 Li ratio is reported as per mil variation, δ 7 Li, from the NIST SRM 8545 Li 2 CO 3 (L-SVEC)standard (Table 11.1). Prior to 1996, Li isotope ratios were often reported as δ 6 Li, i.e., deviations fromthe 6 Li/ 7 Li ratio. However, the standard used was the same, so that for variations less than about 10‰,δ 7 Li ≈ -δ 6 Li; at higher deviations, a more exact conversion is necessary, e.g., -38.5‰ δ 6 Li = 40‰ δ 7 Li.The analytical precision for most of the Li isotope data now in the literature is about 1‰, but recentadvances, particularly the use of multiple-collector inductively coupled plasma mass spectrometers,has reduced uncertainty to as little as 0.2‰.11.6.1 Boron IsotopesIn nature, boron has a valence of +3 and is almost always bound to oxygen or hydroxyl groups in eithertrigonal (e.g., BO 3 ) or tetrahedral (e.g., B(OH) 4 – ) coordination (the only exception is boron bound tofluorine, e.g., BF 3 ). Since the bond strengths and vibrational frequencies of trigonal and tetrahedralforms differ, we can expect that isotopic fractionation will occur between these two forms. This is confirmedby experiments which show a roughly 20‰ fractionation between B(OH) 3 and B(OH) 4 – , with 11 Bpreferentially found in the B(OH) 3 form. In solution, the reaction between trigonal and tetrahedral boronis quite fast, implying equilibrium can be expected and that the isotopic fractionation should reflectthis equilibrium.In natural aqueous solutions boron occurs as both boric acid, B(OH) 3 , and the borate ion, B(OH) 4 – , thedominant species being determined by pH. At pH of around 9 and above, B(OH) 4 – , dominates, at lowerpH B(OH) 3 dominates. In seawater which has a pH in the range of 7.6 to 8.1, about 80-90% of boronwill be in the B(OH) 3 form. Most fresh waters are a little more acidic so B(OH) 3 will be more dominant;only in highly alkaline solutions, such as saline lakes, will B(OH) 4 – be dominant. The most common boronmineral in the crust is tourmaline (Na(Mg,Fe,Li,Al) 3 Si 6 O 18 (BO 3 ) 3 (OH,F) 4 ), in which boron is presentin BO 3 groups. In clays, boron appears to occur primarily as B(OH) 4 – , most likely substituting for silica348 1/9/13

Isotope GeochemistryW, M. White Chapter 11in tetrahedral layers. The coordination of boron in common igneous minerals is uncertain, possiblysubstituting for Si in tetrahedral sites. Boron is an incompatible element in igneous rocks and is veryfluid-mobile. It is also readily adsorbed onto the surfaces of clays. There is an isotopic fractionation betweendissolved and adsorbed B of –20 to -30‰ (i.e, adsorbed B is 11 B poor), depending on pH andtemperature (Palmer et al., 1987).Figure 11.12 illustrates the variation in B isotopic composition in a variety of geologic materials.Spivack and Edmond (1987) found the δ 11 B of seawater was uniform within analytical error. This hasmore recently been confirmed by Foster et al. (2010) who determined a δ 11 B value of 39.61±0.04‰.Fresh mid-ocean ridge basalts have a mean δ 11 B of -4.25±2.1‰. Oceanic island basalts (OIB) haveslightly lighter δ 11 B (e.g., Chaussidon and Jambon, 1994). Bulk chondrites have δ 11 B similar to MORB,which presumably is approximately the bulk silicate Earth value. However, meteoritic materials canhave quite variable δ 11 B as a consequence of avariety of processes, including cosmogenicproduction and decay of 10 Be both in the earlysolar system and subsequent exposure of themeteorites to cosmic rays. The average B isotopiccomposition of the continental crustprobably lies between -13‰ and -8‰ (Chaussidonand Abarède, 1992).Perhaps the most remarkable aspect of B isotopegeochemistry is the very large fractionationof B isotopes between the oceans and thesilicate Earth. It was recognized very early thatthis difference reflected the fractionation thatoccurred during adsorption of boron on clays(e.g., Schwarcz, et al., 1969). However, as wenoted above, this fractionation is only about30‰ or less, whereas the difference betweenthe continental crust and seawater is close to50‰. Furthermore, the net effect of hydrothermalexchange between the oceanic crustand seawater is to decrease the δ 11 B of seawater(Spivack and Edmond, 1987). The discrepancyreflects the fact that the ocean is not a simpleequilibrium system, but rather a kineticallycontrolled open one. Since all processes operatingin the ocean appear to preferentially remove10 B from the ocean, seawater is driven toan extremely 11 B-rich composition. Ishikawaand Nakamura (1993) noted that ancient limestonesand cherts have more negative δ 11 B thantheir modern equivalents, calcareous and siliceousoozes, and suggested that further fractionationoccurred during diagenesis.Another large fractionation occurs duringevaporation and precipitation. Rose-Koga et al.(2006) found that rain and snow is substantiallylighter than seawater with d 11 B ranging from -10 to +34‰. They estimate a seawater–vaporFigure 11.12. Boron isotopic composition in crystallinerocks (MORB: mid-ocean ridge basalts; OIB: oceanicisland basalts; BABB: back-arc basin basalts, IAV: islandarc volcanics), sediments, groundwater, freshwater,salt lakes, seawater, and mid-ocean ridge hydrothermalsolutions.349 1/9/13

Isotope GeochemistryW, M. White Chapter 11fractionation is +25.5‰Spivack and Edmond (1987) investigated the exchange of boron between seawater and oceanic crust.Boron is readily incorporated into the alteration products of basalt, so that even slightly altered basaltsshow a dramatic increase in B concentration and an increase in δ 11 B, with altered oceanic crust havingδ 11 B in the range of 0 to +25‰. Smith et al. (1995) estimated that average altered oceanic crust contains5 ppm B and δ 11 B of +3.4‰. During high temperature interaction between seawater and oceanic crust,Spivack and Edmond (1987) concluded that boron was quantitatively extracted from the oceanic crustby hydrothermal fluids. The δ 11 B of these fluids is slightly lower than that of seawater. They inferredthat the B in these fluids is a simple mixture of seawater- and basalt-derived B and that little or no isotopicfractionation was involved. Analysis of hydrothermal altered basalts recovered by the OceanDrilling Project generally confirm these inferences, as they are boron-poor and have δ 11 B close to 0(Ishikawa and Nakamura, 1992).Island arc volcanics (IAV) have distinctly more positive δ 11 B than either MORB or OIB. This may inpart reflect the incorporation of subducted marine sediment and altered oceanic crust into the sourcesof island arc magmas (e.g., Palmer, 1991), but a more important factor is likely to be fractionation of Bisotopes during dehydration of the subducting slab, in which 11 B is strongly partitioned into the fluidphase (You et al., 1995). This process begins at quite shallow depths in the subduction zone, in theforearc region, where fluids released from the overlying slab serpentinize the forearc mantle and enrichit in 11 B, producing forearc serpentinites with δ 11 B as high as +30‰. By the time the slab reaches thesub-arc magmagenesis region, fluids released are less 11 B-rich, such that island arc volcanics typicallyhave δ 11 B of around +5‰. As Figure 11.12 shows, that the distribution of δ 11 B in island arc volcanics isdistinctly bimodal, with modes at +5‰ and +16‰. All samples with δ 11 B > 12 are from the SouthSandwich arc. Tonarinni et al. (2011) interpret these very high values as a consequence of subductionerosion of the forearc region; i.e., they suggest the strongly 11 B serpentinites of the forearc are being carriedinto the magmagenesis zone.The differences in δ 11 B between oceanic island basalts (OIB) and MORB is perhaps more problematic.Though no experimental or theoretical studies have been carried out, it seems unlikely that significantfractionation of boron isotopes will occur during melting of the mantle, both because the temperaturesare high, and because the atomic environment of B in silicate melts is probably similar to that in silicatesolids. Thus, as we found was the case for O isotopes, B isotope fractionation probably occurs only atthe surface of the Earth, and the difference between OIB and MORB must somehow reflect surfaceprocesses. Chaussidon and Marty (1995) argued that the boron isotopic composition of the mantle isthat of OIB (-10‰) and that the higher δ 11 B of MORB reflects contamination of MORB magmas by alteredoceanic crust. This seems unlikely for several reasons. First, although there are still relatively fewdata available, MORB appear to be relatively homogeneous in their boron isotopic composition. Thismeans assimilation would have to be systematic and pervasive and that all MORB magmas would haveto assimilate roughly the same amount of material. Both of these seem highly improbable. Second,there is little or no other evidence for pervasive assimilation of oceanic crust by MORB magmas. Third,oceanic island basalts have an opportunity to assimilate not only altered oceanic crust, but also overlyingsediment. Yet, according to the Chaussidon and Marty (1995) hypothesis, they are not systematicallycontaminated. Although they are not systematically contaminated, there is evidence of occasionalassimilation of oceanic crust and/or sediment by oceanic island basalt magmas from both B and Os isotopegeochemistry. This may explain some of the lower δ 11 B values in OIB seen in Figure 11.04 (Chaussidonand Jambon, 1994).The alternative explanation for the lower δ 11 B in OIB is that they contain a component of material recycledinto the mantle, through subduction, from the surface of the Earth. The idea that mantle plumes,and the OIB magmas they produce, contain material recycled from the surface of the Earth has beensuggested on other grounds. As we noted above significant fractionation of B isotopes occurs duringsediment dehydration during subduction (You, 1994). The fluid produced will be enriched in 11 B, leav-350 1/9/13

Isotope GeochemistryW, M. White Chapter 11ing the sediment and oceanic depleted in 11 B. Thus the effect of subduction zone processes will be tolower the δ 11 B of oceanic crust and sediment carried into the deep mantle.One of the more interesting applications of boron isotopes has been determining the paleo-pH of theoceans. Boron is readily incorporated into carbonates, with modern marine carbonates having B concentrationsin the range of 15-60 ppm. In modern foraminifera, δ 11 B is roughly 20‰ lighter than theseawater in which they grow. This fractionation seems to result from the kinetics of B co-precipitationin CaCO 3 , in which incorporation of B in carbonate is preceded by surface adsorption of B(OH) –4(Vengoshet al., 1991; Heming and Hanson, 1992).We noted above that boron is present in seawater both as B(OH) 3 , and B(OH) – 4. Since the reaction be-Figure 11.13. Top graph shows the variation pH of surface seawater during Tertiary time as inferredfrom δ 11 B in shells of planktonic foraminifera in ODP cores. Bottom graph shows the concentrationof atmospheric CO 2 calculated from seawater pH. Adapted from Pearson and Palmer (2000).351 1/9/13

Isotope GeochemistryW, M. White Chapter 11tween the two may be written as:The equilibrium constant for this reaction is:B(OH) 3+H 2O ® B(OH) 4 - +H + 11.4-− pK app = ln B(OH) 4− pH 11.5B(OH) 3The relative abundance of these two species is thus pH dependent. Furthermore, we can easily showthat the isotopic composition of these two species must vary if the isotopic composition of seawater isconstant. From mass balance we have:δ 11 B SW = δ 11 B 3 ƒ + δ 11 B 4 (1-ƒ) 11.6−where ƒ is the fraction of B(OH) 3 (and 1 - ƒ is therefore the fraction of B(OH) 4), δ 11 B 3 is the isotopic compositionof B(OH) 3 , and δ 11 −B 4 is the isotopic composition of B(OH) 4. If the isotopic composition of thetwo species are related by a constant fractionation factor, ∆ 3-4 , we can write 11.6 as:δ 11 B SW = δ 11 B 3 ƒ + δ 11 B 4 -δ 11 B 4 ƒ = δ 11 B 4 - ∆ 3-4 ƒ 11.7Solving for δ 11 B 4 , we have:δ 11 B 4 = 11 B SW + ∆ 3-4 ƒ 11.8Thus assuming a constant fractionation factor and isotopic composition of seawater, the δ 11 B of the twoB species will depend only on ƒ, which, as we can see in equation 11.5, will depend on pH.If the mechanism for incorporation of B in carbonate suggested by Vengosh et al. (1991) is correct, thefractionation of 11 B/ 10 B between calcite and seawater will be pH dependent. There is still some debateas to as to the exact mechanism of boron incorporation in carbonate, in particular whether only borateion or both boric acid and borate ion can be incorporated. Regardless of the exact mechanism, the isotopiccomposition of boron in carbonate precipitated from seawater has been shown to be a strongfunction of pH (Sanyal et al., 1996), allowing in principle the reconstruction of paleo-seawater pH fromcarbonates. There are a some additional factors that must be considered: (1) different carbonatesecretingspecies may fractionate B isotopes slightly differently, perhaps because they alter the pH oftheir micro-environment, or perhaps because B(OH) 3 is also utilized to varying degrees, (2) the fractionationfactor is temperature dependent, and (3) the B isotopic composition of seawater may varywith time. Nevertheless, if care is exercised to account for “vital” effects and variation in the isotopiccomposition and temperature of seawater, the B isotopic composition of marine biogenic carbonate preservedin sediment should reflect the pH of the water from which they were precipitated.The pH of seawater, in turn, is largely controlled by the carbonate equilibrium, and depends thereforeon the partial pressure of CO 2 in the atmosphere. Thus if the pH of ancient seawater can be determined,it should be possible to estimate p CO2 of the ancient atmosphere. Given the concern about the relationof future climate to future p CO2 , it is obviously interesting to know how these factors related in thepast.Pearson and Palmer (2000) measured δ 11 B in foraminiferal carbonate extracted from Ocean DrillingProgram (ODP) cores and from this calculated pH based on equations 11.5 through 11.8. To minimizethe effect of temperature on the fractionation factor, they restricted their study to cores from regionsthat were tropical at the time of deposition. To minimize vital effects, they used only 1 species ofplanktonic foraminifera for the Neogene period, G. trilobus (also known as G. sacculifer), which isthought to incorporate B with no vital effect. For the Paleogene, they used 6 species where the vital effectwas arguably minimal. They argue that changes in the B isotopic composition of seawater shouldbe slow to occur since the residence time of B in seawater is roughly 20 million years. Nevertheless,they account for a small variation, roughly 1.7‰, in seawater δ 11 B over Tertiary time. The results suggestdramatically lower seawater pH and dramatically higher p CO2 in the Paleogene. The apparentvariation in p CO2 is qualitatively consistent with what is known about Tertiary climate change – namely352 1/9/13

Isotope GeochemistryW, M. White Chapter 11that a long-term cooling trendbegan in the early to middleEocene. In contrast to thePaleogene, Figure 11.13shows that the Neogene ischaracterized by atmosphericp CO2 near or slightly belowmodern pre-industrial levels.This aspect of the result issomewhat surprising, giventhe evidence for coolingthrough the Neogene,particularly over the last 10-15 Ma (e.g., Figure 10.36). If,as Figure 11.13 suggests,atmospheric p CO2 has beennearly constant through theNeogene, some factor otherthan the greenhouse effectmust account for the coolingover this time.On a more limited timescale, Hönisch and Hemming(2005) investigated δ 11 B overFigure 11.14. a, pCO the last two glacial cycles (0-2 (± uncertainty from δ 11 B measurements at 95%confidence; blue symbols calculated assuming varying [CO -2 3 ], red 140 and 300-420 ka). In thissymbols are for constant [CO -2 3 ]). The grey band is the assumed study, they controlled forthreshold for Antarctic glaciation. b, Deep-sea oxygen isotopes from temperature by analyzing theDSDP site 522 (crosses) and ODP site 744 (diamonds). c, δ 11 B proxy Mg/Ca ratio of the carbonatemeasurements compared to alkenone proxy estimates (green symbols shells, which is know to bewith green shaded band for maximum and minimum).strongly temperaturedependent. Their calculatedpH values ranged from 8.11 to 8.32, which in turn correspond to a p CO2 range of ~180 to ~325 ppm.These calculated p CO2 values are in good agreement with CO 2 concentrations measured in bubbles in theVostok ice core. Hönisch et al. (2009) extended the boron isotope-based pCO 2 record through the Pleistocene.The were particularly interested in the mid-Pleistocene time when the dominant orbital forcingfrequency switched from 40,000 years to 100,000 years. They found that whereas over the last 400,000years pCO 2 has varied from 180 and 300 ppmv in glacial and interglacial periods, respectively, thevariation had been 210 and 280 ppmv in the early Pleistocene. The calculated average pCO 2 of the earlyand late Pleistocene are 248 and 241 ppmv, respectively, and statistically indistinguishable. This a decreasein pCO 2 does not seem to be responsible for the more severe glaciations of the late Pleistocene.Pearson et al. (2009), working with foraminifera from a well-preserved Paleogene section in Tanzaniadetermined pCO 2 over the Oligocene-Eocene transition, a time of great interest because it was then thatAntarctic glaciation began. Some had suspected that a drop in pCO 2 below 750 ppmv may have beenresponsible for the cooling that led to formation of the ice sheet. Their δ 11 B results suggest that pCO 2did dip below this level near this boundary, but recovered in the early Oligocene before declining again(Figure 11.14).Although still somewhat controversial, paleo-seawater pH reconstruction based on boron isotopeshas become better grounded in the last few years. Some of the controversy centered around the lack of353 1/9/13

Isotope GeochemistryW, M. White Chapter 11experimental determination of the fractionation factor between B(OH) 3 and B(OH) 4 – (Pagani et al., 2005;Zeebe 2005). This has be partially resolved by Klochko et al. (2006) who experimentally determined thefractionation factor, α, to be 1.0272± 0.0006 and independent of temperature. This value differs fromthe theoretically estimated value of 1.0194, which had previously been used for paleo-oceanographiccalculations. However, the theoretical is hampered by uncertainties in measured vibrational frequencies,and attempts to calculate it ab initio from molecular orbital theory result in uncertainties that aretoo large to be useful. In addition to this, there are additional uncertainties in the mechanism of incorporationof boron into carbonate and the associated fractionation factor, and uncertainties in how δ 11 Bin seawater has varied with time, and the requirement of high precision measurement of B isotope ratios.Foster (2008) has shown that paleo-CO 2 determined from foraminifera in cores from the Caribbeanagree well with CO 2 in the Vostok ice core using the experimentally determined fractionation factor.11.6.2 Li IsotopesTerrestrial lithium isotopic variation is dominated by the strong fractionation that occurs betweenminerals, particularly silicates, and water. Indeed, this was first demonstrated experimentally by Ureyin the 1930’s. This fractionation in turn reflects the chemical behavior of Li. The ionic radius of Li 1+ issmall (78 pm) and Li readily substitutes for Mg 2+ , Fe 2+ , and Al 3+ in crystal lattices, mainly in octahedralsites. In aqueous solution, it is tetrahedrally coordinated by 4 water molecules (the solvation shell) towhich it is strongly bound, judging from the high solvation energy. These differences in atomic environment,differences in binding energies, the partly covalent nature of bonds, and the low mass of Li alllead to strong fractionation of Li isotopes.Modern study of Li isotope ratios began with the work of Chan and Edmond (1988). They found thatthe isotopic composition of seawater was uniform within analytical error with a δ 7 Li value of +33‰(which has subsequently been revised to +31‰ based on more accurate techniques). Subsequent worksuggests that δ 7 Li in seawater might vary by as much as 4‰, but the degree to which this variation reflectsanalytical error and inter-laboratory biases remains unclear, as the residence time of Li in theocean (1.5-3 Ma) is much longer than the mixing time.Fresh MORB have δ 7 Li of +3.8±1.3‰ (White and Klein, 2013), a range not much larger than thatexpected from analytical error alone. Oceanic island basalts (OIB) have on average higher δ 7 Li:+4.9±1.2‰. The highest δ 7 Li occurs on islands characterized by particularly radiogenic Pb (the socalledHIMU OIB group), such as on some islands of the Cook-Austral chain. Here, δ 7 Li may be as highas +8‰. This may reflect a recycled crustal component in their sources (e.g., Vlastelic et al., 2009). Highprecision analyses of whole carbonaceous and ordinary chondrites have a narrow range of values witha mean of 2.96±0.77‰; enstatite chondrites appear to be systematically lighter, with a mean of1.69±0.73‰ (Pogge von Strandmann, et al., 2011). Individual components of meteorites are more variable.The mean δ 7 Li of fertile, unaltered and unmetasomatized peridotites is +3.5±0.5‰, which is presumablythe value of the bulk silicate Earth, is essentially indistinguishable from that of carbonaceousand ordinary chondrites (Pogge von Strandmann, et al., 2011). Other peridotites exhibit a larger range:-15‰ to +10‰.There appears to be little the relationship between δ 7 Li and other geochemical parameters in igneousrocks, such as MgO concentration, suggesting Li experiences little isotopic fractionation during fractionalcrystallization, and perhaps also partial melting (Tomascak et al., 1999; Teng et al., 2004). However,Pogge von Stratdmann et al. (2011) found a correlation between δ 7 Li and δ 26 Mg in peridotitesxenoliths, which they attribute to kinetic isotope fractionation occurring during transport from themantle. Alpine eclogites can have distinctly light isotopic compositions. These rocks are thought to befragments of basaltic oceanic crust deeply subducted and metamorphosed then subsequently rapidlyexhumed during the Alpine orogeny. Their light isotopic compositions presumably reflect preferentialpartitioning of 7 Li into the fluid produced as the rocks were dehydrated during metamorphism. δ 7 Li in354 1/9/13

Isotope GeochemistryW, M. White Chapter 11granites ranges from about -5 to +10‰, with an average of +1.7‰. Based on this and analysis of othercrustal materials, Teng et al. (2009) estimate the average continental crust to have δ 7 Li = +1.2‰.δ 7 Li in oceanic crust altered by seawater at low temperatures takes up Li from solution and has highδ 7 Li compared to fresh basalt. In hydrothermal reactions, however, Li is extracted from basalt into thesolution and hydrothermal fluids can Li concentrationsup to 50 times greater than seawater.7 Li is extracted more efficiently than6 Li during this process, so hydrothermally alteredbasalt can have δ 7 Li as low as -2‰.Serpentinites (hydrothermally altered peridotite)can have even lower δ 7 Li. Becausethey extract Li from oceanic crust so completely,hydrothermal solutions have Li isotopiccompositions intermediate betweenMORB despite this fractionation.The average δ 7 Li of island arc volcanics,+4.05±1.5‰ is only slightly higher than thatof MORB. This is somewhat surprising sinceother isotopic evidence clearly demonstratesisland arc magmas contain components derivedfrom subducted oceanic crust andsediment. Furthermore, while δ 7 Li have beenshown in some cases to correlate with chemicaland isotopic indicators of a subductioncomponent, this is not always the case.It seems nevertheless likely that the subductionprocess has profoundly influencedthe isotopic composition of the mantle overtime. As a consequence of fractionation occurringduring weathering, seawater isstrongly enriched in 7 Li. This enrichment isimprinted upon the oceanic crust as it reactswith seawater. When the oceanic crust is returnedto the mantle during subduction, themantle becomes progressively enriched in7 Li. The continental crust, on the other hand,becomes progressively depleted in 7 Li overtime. Elliot et al. (2004) calculate that thisprocess has increased δ 7 Li in the mantle by0.5 to 1‰ and decreased δ 7 Li of the continentalcrust by 3‰ over geologic time.As is the case for boron, seawater representsone extreme of the spectrum of isotopiccompositions in the Earth (Figure 11.15).During mineral-water reactions, the heavierisotope, 7 Li, is preferential partitioned intothe solution. Weathering on the continentsresults in river water being isotopicallyheavy, +23.5‰ on average and the sus-Figure 11.15. Li isotopic composition of terrestrial andmeteoritic materials. Diamond represent average values.355 1/9/13

Isotope GeochemistryW, M. White Chapter 11pended load of rivers which have δ 7 Li ≈ +2 (Teng et al., 2004). The riverine flux is slightly smaller thanthe hydrothermal one, which has an average δ 7 Li of +8‰ and the total inputs to seawater are on averageabout +15‰. Thus seawater is some 16 per mil heavier than average river water, so additional fractionationmust occur marine environment. This includes adsorption on particles (although Li is lessprone to absorption than most other metals), authigenic clay formation, and low temperature alterationof oceanic crust. Misra and Froelich (2012) estimate that authigenic clay formation accounts for about70% of Li removal, with alteration of the oceanic crust accounting for the remainder and that the netfractionation factor for these processes is -16‰, consistent with other observations and experiments.δ 7 Li in shale range from -3 to +5‰. Marine carbonate sediments, which tend to be Li-poor, typicallyhave higher δ 7 Li than non-carbonate sediment.Misra and Froehlich (2012)compiled lithium isotopicanalyses of Cenozoic foraminiferaand have shown theδ 7 Li of seawater has inincreasedby 9‰ over thisperiod. Although notidentical, it tracks the rise in87 Sr/ 86 Sr and187 Os/ 188 Osremarkably well (Figure11.16). Misra and Froehlichattribute the change in allthree ratios to changes inweathering of the continentsdue primarily to changes intectonism over the Cenozoic,which has seen the rise of theRocky Mountains, theAndes, the Himalayas, andthe Alps. As they point out,low-lying terrains whereremoval of weatheringproducts is transportlimited,especially those inthe tropics, undergo congruentweathering Li isotope ratiosthat reflect their bedrocks.Mountainous terrainswith weathering undergohigh weathering and denudationrates with incongruentweathering, and largerates of secondary clay formationand hence dissolvedLi is 7 Li-enriched. The significanceof this is the importantrole that silicate weatheringplays in drawing downatmospheric CO 2 . They noteFigure 11.16. δ 7 Li, 87 Sr/ 856 Sr, and 187 Os/ 188 Os in seawater over the Cenozoic.From Misra and Froehlich (2012).356 1/9/13

Isotope GeochemistryW, M. White Chapter 11the overall similarity of these curves to that of ocean bottom water δ 18 O, which records decreasing temperatureand increasing ice volume. They suggest “δ 7 Li SW might provide alternative estimates of atmosphericCO2 consumption by the silicate weathering.”Rudnick et al. (2004) found that a saprolite * developed on granite had a lighter isotopic composition(as light as -6.8‰) than the granite (+2.3‰). δ 7 Li decreased with decreasing Li concentration in a mannerconsistent with leaching of Li by Rayleigh fractionation during weathering with a ∆ residue-solution of -3‰. Far more negative values were observed in saprolite developed on a diabase, with δ 7 Li as low as -20‰. Again, Li decreased with decreasing concentration consistent with Rayleigh fractionation, but thesaprolite also likely gained Li from isotopically heavy groundwater.Diffusion can also fractionate Li isotopes. As we noted earlier in an earlier chapter, lighter isotopes ofan element will diffuse faster than heavier isotopes. The relatively large mass difference between 7 Liand 6 Li (17%) results in substantially faster diffusion of 6 Li. Richter et al. 1999) found that the ratio ofdiffusion coefficients for isotopes of an ion diffusing in molten silicates obeyed the relation:D 1⎛= m ⎞2D 2 ⎝⎜⎠⎟m 1β11.08where β is an empirical parameter determined experimentally. Richter et al. (2003) found that the valueof β was 0.215 for Li, implying 3% faster diffusion of 6 Li. In molten basalt-rhyolite diffusion experiments,this more rapid diffusion of 6 Li produced isotopic variations as great as 40‰ over 10 mm distancesin 15 hours. Comparable isotopic variations have been observed in nature. Teng et al. (2006) observedthat the isotopic composition of Li diffusing out of a pegmatite into surrounding amphibolitedecreased from +7.6‰ to -19.9‰ over a distance of 10m. Because of its small ionic size and charge, Lidiffuses more readily than most other elements. Indeed, Richter et al. (2009) found it diffused 2 ordersof magnitude faster than Ca. This rapid diffusion also contributes to the large potential for the diffusionalisotopic fractionation.11.7 ISOTOPES OF MAGNESIUM AND CALCIUMCalcium and magnesium are alkaline earth elements and exist in nature almost exclusively in the +2valance state. Magnesium is the third most abundant element; calcium is the fifth. Both are lithophile,mobile, and fairly soluble (they are among the most abundant cations in natural waters), and both areconservative ions in seawater, which is to say their concentrations vary only in proportion to salinity.Both are bio-essential elements and are taken up by organisms in significant quantities, but abundantenough that they are rarely, if ever, biolimiting. Mg is incorporated into the chlorophyll molecule and isinvolved in energy metabolism and protein synthesis. Ca is widely used by organisms in structural tissuessuch as bones and shells, and plays key roles in regulating a variety of cellular processes and in intercellularcommunication such as neurotransmission. These elements form carbonates more readilythan most other elements and these carbonates form a significant fraction of the sedimentary mass.11.7.1 Mg IsotopesMg has three stable isotopes: 24 Mg, 25 Mg, and 26 Mg with relative abundances of 78.99%, 10.00%, and11.01%, respectively (Cousey et al., 2011). We have already seen that 26 Mg is the radiogenic product ofthe short-lived radionuclide, 26 Al, and that the 26 Al- 26 Mg is the most important chronometer of events inthe early solar system. However, variations in 26 Mg due to radioactive decay are restricted to the earliestformed objects in the solar system, CAI’s and chondrules; subsequently formed objects, such as meteoriteparent bodies and planets, appear to be homogeneous with respect to radiogenic 26 Mg, and ourfocus in this chapter will be on variations in Mg isotope ratios resulting from chemical fractionations.* Saprolite is highly weathered rock that constitutes the base of a soil profile (the C horizon).357 1/9/13

Isotope GeochemistryW, M. White Chapter 11By convention, the isotope ratios of interest are 25 Mg/ 24 Mg and 26 Mg/ 24 Mg and these are reported inthe usual notation indicating per mil deviations from a standard, δ 25 Mg and δ 26 Mg, respectively. Therehas, however, been some evolution in this notation. Initially, interest in Mg isotopes focused exclusivelyon radiogenic 26 Mg and the symbol δ 26 Mg referred to variations in 26 Mg due to decay of 26 Al and not tomass fractionation. Mass fraction effects were expressed as ∆ 25 Mg (per mil deviations of 25 Mg/ 26 Mg). Inorder to be consistent with notation used for other elements, current notation uses δ 26 Mg to refers tovariations due to mass fractionation, δ 26 Mg* refers to radiogenic variations in 26 Mg, and ∆ 25 Mg is usedto reserved for mass independent fractionations in a manner exactly analogous to ∆ 17 O and ∆ 33 S. However,no mass independent fractionations of Mg isotopes have yet been observed in terrestrial materials,and δ 25 Mg ≈ 0.52 δ 26 Mg. Prior to 2003, Mg isotope data was reported relative to a purified magnesiummetal standard, NIST-SRM 980; however, that standard proved to be isotopically heterogeneous andthe current standard is a solution designated DSM3, derived from Mg extracted from the Dead Sea.Data can be approximately converted using δ 26 Mg DSM3 = δ 26 Mg SRM980 + 3.405 (the exact conversion isgiven by Young and Galy, 2004). Our discussion here will focus exclusively on δ 26 Mg DSM3 .Schauble (2011) has calculated fractionation factors for a variety of minerals as well as aqueous solutionfrom partition function using the theoretical approach described in Chapter 7. These can be approximatedusing the following polynomial approximation:Figure 11.17. 26 Mg/ 24 Mg fractionation factors for a variety of mineralsas well as Mg 2+ ion in aqueous solution calculated from the polynomialequation given by Schauble (2011).1000lnα = AT + B6 T + C 4 T 11.092where T is thermodynamic temperature and A, B, and C are constants unique to each pair of phases.Calculated values are shown plotted as a function of temperature in Figure 11.17. The results indicatethat we expect heavy Mg isotopes to partition in the order aluminate/oxides> silicates> water> carbonate.Particularly strong fractionationis predicted to occurat low temperature betweenwater and/or silicates and carbonate,with the carbonatebecoming isotopically light. Athigher temperatures, fractionationamong mantle silicates(olivine and pyroxenes) is predictedto be quite small, with ∆values less than 0.1‰ above800˚C; however significantfractionation of >0.5‰ is predictedto occur between silicatesand non-silicates such asspinel even at temperaturesabove 1000˚C. The coordinationof Mg in spinel is, ofcourse, quite different than insilicates, so a relatively largefractionation is not surprising.Figure 11.18 shows the variationof δ 26 Mg in terrestrial materialsand bulk meteorites.Fresh peridotites have δ 26 Mg =-0.22±0.07‰ and shows no re-358 1/9/13

Isotope GeochemistryW, M. White Chapter 11solvable variation with composition. Thisvalue presumably represents the isotopiccomposition of the bulk silicate Earth andis indistinguishable from the average valuefor basalts (-0.26±0.07‰), which also showno resolvable variations with composition.Chondrites have a mean δ 26 Mg of-0.28±0.06‰ and show no systematic variationsbetween classes (Teng et al., 2010;Pogge von Stradmann et al., 2011). Thissuggests Mg isotope fractionations at hightemperature and in magmatic systems are,overall, insignificant and is consistent withour expectations based on Schauble’s(2011) calculated partition coefficients.In spite of the apparent uniformity in Mgisotopic composition of bulk mantle samplesand basalts, measurable variations onthe mineral grain scale have been observed.Young et al. (2009) demonstratedδ 26 Mg differences between spinel (MgAlO 4 )and olivine in San Carlos peridotite xenolithsof up to 0.88‰ (spinel being isotopicallyheavier), which were consistent withtheoretically predicted fractionations at800˚C. Spinel abundances are generallyquite low in peridotites (< 1% in thosestudied by Young et al.), so it would contributeonly negligibly to Mg isotope fractionationduring melting. Nevertheless, Mgisotope fractionation between spinel-olivinepairs has potential as a geothermometerwhen the analyses can be donewith sufficient precision. Differences betweenolivine and pyroxenes were smaller,on the order of 0.2 to 0.3‰, but still largerthan the theoretically expected fractionation,suggesting Mg isotopic disequilibrium.Teng et al. (2011) reported correlatedvariation in δ 26 Mg and δ 56 Fe in olivinefragments of a Hawaiian basalt, with δ 56 Fe Figure 11.18. Magnesium isotopes in terrestrial materials.The 2σ variation in peridotites, seawater, OIB, and= -3.3 × δ 26 Mg. The variation (total variationin δ 26 Mg was up to 0.4‰) correlated MORB are less than the size of the symbols. Data forwith the Mg/(Mg+Fe) ratio of the olivines peridotites, MORB, OIB, and chondrites are from Tengand Teng et al. (2011) interpreted the et al., (2010). Flux-weighted average riverine δ 26 Mg isvariations are resulting from diffusiondrivenfractionation as the olivine re-shown by the arrow and is from Tipper et al. (2006).equilibrated with the surrounding cooling magma.359 1/9/13

Isotope GeochemistryW, M. White Chapter 11In contrast to basalts and peridotites, continental materials and natural waters show measurablevariation in δ 26 Mg. Granites vary in δ 26 Mg from -0.3 to 0.44‰. This variation is unrelated to SiO 2 contentand hence apparently reflects variation in source composition, which can include sediments anddeep crustal materials, rather than igneous differentiation. Li et al. (2010) found that S-type (derivedfrom melting of metasediments) and I-type (derived from melting of meta-igneous rocks) has a relativelynarrow range of isotopic compositions and were on average only slightly isotopically heavierthan the bulk silicate Earth. A-type granites from China, derived by deep crustal anatexis, tended to beheavier and more isotopically variable. Granites from the Peninsular Range (Baja California) are evenheavier, with δ 26 Mg up to +0.44‰ (Shen et al., 2009). The mean δ 26 Mg of granites is -0.08‰, somewhatheavier than the bulk silicate Earth value.Non-carbonate sediments show a wider variation of from about -0.5 to +0.9‰ and have an averageδ 26 Mg of 0‰. The greatest variation, however, is between carbonate and silicate materials; there is essentiallyno overlap between carbonate and silicate materials, which is consistent with the large differencein coordination and bonding of Mg and predicted fractionation factors. There is considerablevariation among carbonates, which range from δ 26 Mg of -1‰ to -5‰. Some or much of this variationappears to be mineralogically controlled with δ 26 Mg decreasing in the order dolomite>aragonite>highmagnesium calcite>low magnesium calcite (Hippler et al., 2009). Skeletal carbonates appear to showadditional variation related to phylum, although within foraminifera interspecific variation in appearslimited (Pogge von Strandmann, 2008). For the most part, Mg isotopic variations in skeletal carbonateappear to be independent of temperature and salinity.Rivers also show a wide isotopic variation that reflects the δ 26 Mg of their drainage basin: most rivershave δ 26 Mg in the range of -1.5‰ to +0.5‰, but those draining carbonate terrains can have δ 26 Mg

Isotope GeochemistryW, M. White Chapter 11other potentially important sink are dolomite precipitation and, possibly, exchange reactions with clays(in which Mg 2+ in solution replaces Ca 2+ and other ions in clays), although the latter is likely to be minor.Unfortunately, there are as yet no empirical or theoretical of fractionation factors for ion exchangereactions with clays, but both exist for dolomite precipitation. Dolomites show a fairly wide range ofMg isotopic compositions, but using the mean δ 26 Mg value of -2‰, Tipper et al. (2008) estimate that87% of seawater Mg is removed by hydrothermal systems and 13% by dolomite precipitation.Over the long term, Mg isotopic composition of seawater depends on (1) the riverine flux and its Mgisotopic composition, which in turn depends on the weathering rates, (2) the hydrothermal flux, whichin turn depends on the rate of seafloor-spreading, and (3) the rate of dolomite formation. All three ofthese factors are likely to vary over geologic time. The question of rates of dolomite formation is interestingbecause judging from the amount of dolomite in the sedimentary mass, the present rate of formationappears to be slow compared to the geologic past. While the rates of seafloor spreading over thelast 100 Ma can constrained from magnetic anomaly patterns, the degree to which these rates have variedare nonetheless debated, and independent constraints would be useful. Finally, weathering ratesdepend on both climate (temperature, precipitation) and atmospheric CO 2 concentrations. There is intenseinterest in how these factors have varied. If the Mg isotopic composition of seawater through geologictime could be established, it could be potentially useful in addressing all these issues. The δ 26 Mgof foraminiferal shells appears to be independent of temperature and water chemistry and thus mightprovide a record of δ 26 Mg through time. However, it must first be established that Mg isotopic compositionsof forams (or any other potential recorder of seawater δ 26 Mg) do not change through diagenesis.The question of inter-species differences would also have to have to be addressed. There are a host ofother issues as well. For example, what controls Mg isotopic fractionation during weathering, whatcontrols isotopic fractionation during dolomite formation, etc.11.7.2 Calcium IsotopesCalcium has six stable isotopes: 40 Ca, 42 Ca, and 43 Ca, 44 Ca, 46 Ca, and 48 Ca with relative abundances of96.94%, 0.647%, 0.135%, 2.086%, 0.0004%, and 0.187%, respectively (Cousey et al., 2011). 40 Ca is the principaldecay product of 40 K (89.5% of 40 K decays). However, because 40 Ca is vastly more abundant than40 K, variation in 40 Ca due to radioactive decay is generally less than 0.01% (K-rich/Ca-poor materials,such as salt deposits, are an exception). Chemical fractionations of Ca isotope ratios are thus the principalinterest. Unfortunately, there are several ways of reporting calcium isotope variations. The olderconvention is to measure the 44 Ca/ 40 Ca ratio and reported it as δ 44 Ca (or δ 44/40 Ca). There are two difficultieswith this approach: (1) the 44 Ca/ 40 Ca ratio is small, ~0.02, and is difficult to measure accurately, and(2) some variation in 40 Ca abundance results from radioactive decay of 40 K. The latter point is illustratedby a study by Ryu et. al. (2011), who found that δ 44/40 Ca in various minerals of the Boulder Creek granodioritesvaried by 8.8‰ (K-feldspar had the highest δ 44/40 Ca) while δ 44/42 Ca values varied only by0.5‰. Consequently, a second convention has emerged, which is to measure the 44 Ca/ 42 Ca ratio, reportedas δ 44/42 Ca. Because Ca is such an abundant element, relatively little is sacrificed by measuringthe less abundant isotopes.No consensus has entirely emerged on what standard value should be used for the delta notation.Many labs report values relative to the NIST SRM 915a CaCO 3 standard (which is widely used as astandard), whose isotope ratios is listed in Table 11.1. However, there are exceptions to this convention;UC Berkeley reports ratios relative to bulk silicate Earth, whose composition relative to NIST SRM 915ais δ 44/40 Ca SRM915a = +0.97‰, δ 43/40 Ca SRM915a = +0.88‰, and δ 44/42 Ca SRM915a = +0.46‰. Other labs report valuesrelative to seawater, whose isotopic composition is δ 44/40 Ca SRM915a = 1.88±0.04‰ and δ 44/42 Ca SRM915a =0.94±0.07‰ (Hippler et al., 2003). SRM 915a is no longer available and has been replaced by SRM 915bwhose δ 44/40 Ca SRM915a = +0.72±0.04‰ and δ 42/44 Ca = +0.34±0.02‰. Studies to date suggest that all observedcalcium isotope fractionations are mass dependent: in other words, δ 44/40 Ca, δ 43/42 Ca, and δ 44/42 Caare strongly correlated and the other two ratios can be predicted from measuring any one (excepting361 1/9/13

Isotope GeochemistryW, M. White Chapter 11any radiogenic variations in 40 Ca). Consequently, δ 44/42 Ca ≅0.476 × δ 44/40 Ca. An overview of calcium isotopiccomposition of terrestrial and extraterrestrial materials isshown in Figure 11.19.Simon and DePaolo (2010) found that the Earth, Moon,Mars, and differentiated asteroids (4-Vesta and theangrite and aubrite parent bodies) have δ 44/40 Ca that isindistinguishable from primitive ordinary chondriticmeteorites, while enstatite chondrites are 0.5‰ enrichedand primitive carbonaceous chondrites 0.5‰ depletedrelative to ordinary chondrites. They speculate that thevariations observed in enstatite and carbonaceouschondrites reflect fractionation during high temperatureevaporation and condensation in the early solar nebula.These initial variations were averaged out in duringaccretion of large bodies such as asteroids and planets.To date, there has been only a limited effort toinvestigate Ca isotope fractionations in terrestrial igneousrocks; δ 44/40 Ca values compiled by DePaolo (2004) show arange of nearly 0.7‰, some of which reflects variableamounts of radiogenic 40 Ca; the small number of igneousrock δ 44/42 Ca SRM915a values in the literature range from+0.31‰ to +0.80‰. Individual minerals show greatervariation. As noted above, minerals from a singlegranodiorite studied by Ryu et al. (2011) varied by(0.5‰). Huang et al (2010) found that δ 42/44 Ca in orthopyroxenewas 0.38‰ higher that clinopyroxene inKilbourne Hole peridotites xenoliths and 0.25‰ higher inSan Carlos peridotite xenoliths. They estimated theδ 44/40 Ca SRM915a of the Earth’s mantle to be +1.05‰(δ 44/42 Ca SRM915a = +0.50‰), slightly higher than the averageratios they measured in basalts (δ 44/40 Ca SRM915a = +0.97±Figure 11.19. Ca isotopic compositionof terrestrial and meteoritic materials.Isotopic compositions of biogenic carbonatesare shown in red. Arrowshows the average composition of continentalrunoff of Tippler et al. (2010).0.04‰) and slightly higher than the UC Berkeley bulk silicate Earth value (δ 44/40 Ca SRM915a = +0.97‰).Huang et al. (2011) analyzed Hawaiian lavas and found that δ 42/44 Ca SRM915a in lavas of Koolau volcano(Oahu) were much lower: 0.34 to 0.40‰ and found that calcium isotope ratios correlated inversely with87 Sr/ 86 Sr (Fig 11.20) and with Sr/Nb ratios, but not with other trace element ratios. Huang et al. arguedthat the calcium isotope variations and these correlations reflected the presence of marine carbonates inancient recycled oceanic crust that makes up part of the Hawaiian mantle plume (e.g., Hofmann andWhite, 1982; Sobolev et al., 2005).High temperature hydrothermal fluids have a δ 44/40 Ca SRM915a of +0.95‰, well within the range of theisotopic composition of MORB, thus there appears to be no significant isotopic fractionation betweenhydrothermal fluids and oceanic crust (Amini et al., 2008). However, hydrothermal systems alsoinvolve precipitation of anhydrite and Amini et al. (2008) found the fractionation factor (∆ 44/40 Ca) foranhydrite precipitation in oceanic crust to be -0.5‰. In addition, aragonite precipitates within theoceanic crust at low temperatures with similar fractionation factors (-0.34‰). Thus the effect of seawaterinteraction with the oceanic crust is to drive seawater to heavier isotopic compositions.362 1/9/13

Isotope GeochemistryW, M. White Chapter 11Several studies have shown thatthere is apparently little fractionationduring physical weathering, at leastduring early stages. In laboratorydissolution experiments Ryu et al.(2011) found that δ 42/44 Ca of solutionsproduced in the experiments varieddue to incongruent dissolution, butthat little mass fractionationoccurred. Hindshaw et al. (2011)found that soils that have developedover the last 150 years in front of theretreating Damma glacier inSwitzerland has Ca isotopic ratiosidentical to the granite on which theyhad developed. In contrast to purelyphysical weathering, significantfractionations occur when biology isinvolved. Plants preferentially takeup lighter Ca isotopes; Weigand et al.(2005) found that calcium uptake byHawaiian Ohia trees has ∆ 44/40 Cafractionation factors of -1 to -2‰; oneFigure 11.20. δ 44/42 Ca SRM915a vs. 87 Sr/ 86 Sr in Hawaiian lavasanalyzed by Huang et al. (2011). Huang et al. interpreted thiscorrelation as mixing between recycled sedimentary carbonateand mantle.the other hand, twigs and leaves are about 0.5‰ heavier than the Ca in xylem. As a result of this preferentialuptake of light Ca isotopes by the flora, the soil solutions become isotopically heavier (e.g.,Cenki-Tok et al. 2009). In the marine environment, autotrophs such as the alga Emiliania huxleyi alsopreferentially utilize isotopically light Ca. E. huxleyi is a coccolithophorid and secretes a test, or shell,composed of calcite plates or coccoliths, which constitute about half the calcium carbonate precipitatedfrom the ocean. Such precipitation is, of course, and important part of the global calcium cycle and weconsider it next.Significant fractionation occurs in precipitation of calcium carbonate from solution. Marriott et al(2004) found the ∆ 44/42 Ca fractionation factor for inorganic calcite precipitation had a temperature dependenceof 0.008±0.005‰/˚C (∆ 44/40 Ca = 0.015‰/˚C). Gussone et al. (2005) found that the temperaturedependence of the fractionation factor for aragonite was similar to that of calcite, but that the fractionationfactor for aragonite was about 0.6‰ lower than for calcite at any given temperature. In addition totemperature, the fractionation factor appears to depend on CO 3 2- concentration, precipitation rate, andMg 2+ concentration, with less fractionation in the precipitation of high-magnesium calcite.Most calcium carbonate precipitation is biogenic. Gussone et al. (2006) found that fractionation factorfor precipitation of E. huxleyi coccoliths was greater than that for inorganic precipitation but that for thetemperature dependence ∆ 44/40 Ca fractionation factor (0.027±0.006‰/˚C) was similar to the temperaturedependence for inorganic calcite precipitation. Growth rate, carbonate concentrations, and otherfactors appeared to have little effect on the fractionation factor. They also noted that the isotopic compositionof the whole organism is essentially identical to that of the calcite coccoliths and therefore thatthe fractionation apparently occurs during uptake of Ca from seawater rather than during calcite precipitation.Ca isotope fractionation by planktonic foraminifera, which also secrete calcite tests, does notshow simple temperature dependence.363 1/9/13

Isotope GeochemistryW, M. White Chapter 11While Gussone et al., (2003) found thatΔ 44/40 Ca exhibited a temperature dependence of0.24‰/˚C in laboratory-grown Globigerinoidessacculifer, subsequent studies at lower salinityfound no temperature dependence (Gussone etal., 2009). Sime et al. (2005) found no significanttemperature dependence in the Ca isotopiccomposition of tests of 12 planktonic speciesrecovered from deep-sea core tops. It appearsthat any temperature-dependence of Ca isotopefractionation in planktonic foraminifera fractionationis masked by other factors such assalinity and kinetic fractionations related togrowth rate (Kisakürek et al., 2011). Temperaturedependence of the fractionation factorin benthic foraminifera also appears weak,particularly below 5˚C (Gussone andFlippsone, 2010). Table 11.2 lists the approximatefractionation factors for biogenic carbonateprecipitation. Scleractinian corals (e.g.,reef-building corals) are anomalous in that although they precipitate aragonite, fractionation factors aresimilar to those for calcite secreting organisms (Böhm et al., 2006).In animals, Ca isotope systematics are complex. The isotopic composition of soft tissues (muscle,blood) appears to track that of diet, althoughwith considerable variability (Figure 11.21).In chickens, for example, Skulan andDePaolo (1999) found that δ 44/40 Ca varied bymore than 3‰ between blood, muscle, eggwhite, and egg yolk, with egg white and eggyolk differing by nearly 2‰. Mineralized tissues(bones, shell, teeth) were on averageabout 1.3‰ lighter than soft tissues. Subsequentstudies (e.g., Chu et al., 2006) havegenerally confirmed this effect. The datasuggest that in animals there is little Caisotopic fractionation in uptake but a largefractionation in mineralized tissue formation.Soft tissues are more variable and this variabilitylikely reflects both fast cycling andshort residence times of calcium ion in softtissues as well as two-way exchange of Cabetween soft and mineralized tissues. In addition,Reynard et al. (2010) found that insheep, ewes had δ 42/44 Ca about 0.14‰ higherthan rams. Noting the very light isotopiccomposition of sheep’s milk relative to theirdiet (Chu et al., 2006), they attributed thissexual difference to lactation in ewes.Table 11.2 Calcium Isotope Fractionationin Biogenic CarbonateFractionation FactorsOrganism ∆ 44/40 Ca ∆ 44/42 CaBivalves (calcite) -1.50 -0.71Foraminifera (calcite) -0.94 -0.45Coccolithophorids (calcite) -1.30 -0.62Brachiopods (calcite) -0.85 -0.40Sponges (aragonite) -1.50 -0.71Pteropod snails (aragonite) -1.40 -0.67Scleractinian corals(aragonite)-1.10 -0.52Figure 11.21. Relationship between δ 44/40 Ca in diet andsoft and mineralized tissues in animals. After Skulan andDePaolo (1999).364 1/9/13

Isotope GeochemistryW, M. White Chapter 11Figure 11.22. Ca isotopic composition of seawater over the last 500 Ma calculated from the isotopiccomposition of marine carbonates and phosphates. Red line shows a 10-point moving average; darkand light grey regions show the 1σ and 2σ bounds, respectively. After Farkaš et al. (2007).Farkas et al. (2007) attempted to deduce the Ca isotopic history of seawater over Phanerozoic timefrom the isotopic composition of marine carbonates and phosphates (Figure 11.22). The results suggestthat δ 44/42 Ca has increased by ~0.33‰ over the last 500 Ma, although the path has been bumpy. An increasein the Carboniferous was followed by a return to lower values in the Permian and Triassic. Althoughdetails are unclear because of sparse data coverage, values again increased in the second half ofthe Mesozoic and declined again in Paleogene before increasing to present values in the Neogene.Farkaš et al. concluded that not only must have Ca fluxes changed over time (there is independent evidencefrom fluid inclusions in evaporites that seawater Ca concentrations have changed with time), butfractionation factors must have changed as well. They proposed that this varying fractionation reflectedvariation in the dominant mineralogy in marine carbonate precipitations: oscillating between calciteand aragonite. In their hypothesis, that in turn reflected variation in the oceanic Mg/Ca ratio: lowMg/Ca favors calcite while high Mg/Ca favors aragonite. They suggest that the Mg/Ca ratio was inturn controlled by tectonic processes, specifically variable rates of oceanic crust production that modulatedthe hydrothermal calcium and magnesium flux to and from the oceans. Sime et al. (2007) reconstructedthe marine Ca isotope record over the last 24 million years using planktonic foraminifera. Theyconcluded that variations in calcium flux and ∆ 44/42 Ca during calcite precipitation were insufficient toaccount for the variation in δ 42/44 Ca observed (about 0.1‰), although they played a role. They concludedthat variations of ±0.05‰ in the isotopic composition of weathering flux was required.11.8 SILICON ISOTOPESSilicon, which is the third or fourth most abundant element on Earth (depending on how much maybe in the core), has three isotopes: 28 Si (92.23%), 29 Si (4.69%), and 30 Si (3.09%) (Coursey et al., 2012). By365 1/9/13

Isotope GeochemistryW, M. White Chapter 11convention, 29 Si/ 28 Si and 30 Si/ 28 Si ratios are reportedas δ 29 Si and δ 30 Si relative to the standardNBS28 (NIST-RM8546) whose isotopiccomposition is 30 Si/ 28 Si = 0.033532 and 29 Si/ 29 Si= 0.0508204 (Coplen et al., 2002). The first studyof silicon isotope geochemistry is 60 years old(Reynolds and Verhoogen, 1953), but the fieldhas rapidly expanded only since the advent ofthe high-precision multi-collector-ICP-MS inthe last decade or so, and some aspects of Siisotope geochemistry are not yet fully understood.To date, all reported δ 29 Si and δ 30 Si areconsistent with mass-dependent fractionation,so we will consider only δ 30 Si.Figure 11.23 provides an overview of the Siisotopic composition of terrestrial andextraterrestrial materials. Silicon isotopegeochemistry has relevance to a wide variety ofissues in earth science. The first, and arguablythe most fundamental of these, is the parentalmaterial of the Earth and the composition ofthe Earth’s core. As we saw in Chapter 5, theEarth and Moon uniquely share a commonoxygen isotopic composition with enstatitechondrites. This has led some to suggest thatenstatite chondrites provide a better model forthe Earth’s composition than carbonaceous orordinary chondrites (e.g., Javoy et al., 2010).Estimates of the δ 30 Si of the bulk silicate Earthvary from -0.29±0.08‰ (Savage et al., 2010) and-0.28±0.05‰ (Fitoussi et al., 2009) to -0.38‰(Chakrabarti & Jacobsen, 2010). Excepting thelatter estimate ‡ , this value falls outside therange observed in ordinary and carbonaceouschondritic meteorites (—0.36 to -0.56‰) andmuch outside that of enstatite chondrites (-0.58to -0.67‰) (Chakrabarti & Jacobsen, 2010;Armytage et al., 2011). The Moon appears tohave the same Si isotopic composition as thesilicate Earth (Fitoussi and Bourdon, 2012;Armytage et al., 2012). There is good agreementthat the difference in Si isotopic compositionbetween meteorites (representing nebular materialparental to the Earth) and the bulk silicateEarth reflects isotopic fractionation of Si be-Figure 11.22. Silicon isotopic composition of terrestrialand solar system materials. Dashed line isthe estimated δ 30 Si of the bulk silicate Earth. “C &O chondrites” are carbonaceous and ordinarychondrites; “E chondrites” are enstatite chondrites;grey area shows the range of δ 30 Si in seawater;solid line is estimated average seawatercomposition. Arrow shows estimated averagecomposition of rivers. Precambrian cherts fromcompilation of Chakrabarti et al., 2012).‡ Here we exclude the value of Chakrabati and Jacobsen (2010) and adopt a δ 30 Si value for the bulk silicate Earth of-0.29‰ because the values of international analytical standards reported by Chakrabati and Jacobsen (2010) differsignificantly from those reported by other laboratories.366 1/9/13

Isotope GeochemistryW, M. White Chapter 11tween the core and silicate Earth. Observational differences of Si isotopic composition between metaland silicate phases in enstatite chondrites (Ziegler et al., 2010), experimental data (Shalar et al., 2011),and theoretical calculations (Schauble et al., 2007) indicate that the fractionation of Si isotopes betweenmetal and silicate can be expressed as:∆ 30 Si silicate−metal≅7.5 ×106T 2 11.10This equation tells us that isotopically light Si preferentially partitions into the metal phase (i.e., thecore) and the extent of fractionation decreases with temperature. We don’t know exactly the temperatureof equilibration, but assuming a difference in δ 30 Si between the bulk silicate Earth and carbonaceousor chondrites of -0.15‰, Armytage et al. (2011) concluded that the core contains ~8.7 wt% Siwhile Ziegler et al. (2010) concluded the core contains at least 6% Si. This amount of Si would be consistentwith geophysical observations, such as seismic velocity and moment of inertia, that constraint thedensity of the core are require that it contain a few percent of an element lighter than Fe or Ni. Fitoussiand Bourdon (2012) calculate that to account for the much greater difference in δ 30 Si between the Earthand Moon and enstatite chondrites, the Earth’s core would have to contain 28 wt% Si, an amount muchgreater than allowed by geophysical constraints. The similarity of δ 30 Si of the Moon and silicate Earthimplies that the Earth’s core had mostly segregated before the Moon-forming impact and the δ 30 Si insilicates from proto-Earth and the impactor were homogenized in the aftermath of the impact (Armytageet al., 2012). Considering Si, Cr, Ni, and O isotopic compositions, Fitoussi and Bourdon (2012) suggestthat the Earth-Moon composition could be accounted for if the parental material were a mix of carbonaceousand ordinary chondritic material with the addition of 15% of enstatite chondrite.The average δ 3- Si of mantle-derived ultramafic xenoliths is -0.30±0.04‰, that of basalts is-0.28±0.03‰, and that of granitic rocks is -0.23±0.13‰. This implies that there is a slight fractionationassociated with melting and fractional crystallization, with lighter silicon isotopes partitioning preferentiallyinto SiO 2 -poor mafic minerals such as olivine. Savage et al. (2012) found that δ 30 Si in igneousrocks depended on SiO 2 composition approximately as:δ 30 Si(‰) = 0.0056 × [SiO 2]− 0.56811.12Savage et al. (2012) also found a slight variation in δ 30 Si in granites that related to their petrogenesis: S-type granites (those derived by melting of sedimentary precursors and with Al 2 O 3 /(CaO+Na 2 O+K 2 O)>1) had slightly lighter δ 30 Si than either I-type (derived from melting of igneous precursors) or A-type (derived by fractional crystallization of a mafic parent magma) granites. Compared to other processes,however, Si isotope fractionation in igneous processes is quite small; for example, in the course ofevolution from basaltic to andesitic, the δ 30 Si of a magma would increase by only ~0.06‰, an amountonly slightly greater than present analytical precision. This, of course, should not be surprising because(1) temperatures involved are high, (2) the oxidation state of Si does not vary, and (3) the atomic environmentsof Si in silicate minerals and melts do not differ greatly.At lower temperatures and where another form of Si is involved (silicic acid: H 4 SiO 4 ), fractionationsare (not surprisingly) greater. Igneous minerals at the surface of the Earth undergo weathering reactionssuch as:2NaAlSi 3 O 8 + 5H 2 O → Al 2 Si 2 O 5 (OH) 4 + 3SiO 2 + 2Na + + 2OH – + H 4 SiO 4Thus when albite reacts with water, Si partitions between residual clay (kaolinite in this example),quartz, and silicic acid in aqueous solution. This is an overall reaction that involves a variety of intermediatesteps and phases and furthermore occurs rather slowly. Thus determining the fractionationfactors for such reactions experimentally is difficult. Méhuet et al. (2007) used a theoretical approach tocalculate a ∆ 30 Si kaolinite-quartz fractionation factor of -1.6‰ at 25˚C. Experimental estimates of thefractionation of between dissolved H 4 SiO 4 and biogenic opaline silica indicate that ∆ 30 Si opal-diss. Si ≈ -1.1‰367 1/9/13

Isotope GeochemistryW, M. White Chapter 11(De la Rocha et al., 1997). Other studies indicate little fractionation in the transformation of opal toquartz, so we can infer that the fractionation between kaolinite and dissolved silica should be ~ -2.5‰.Consequently, we expect that weathering of silicate rocks to produce isotopically light clays and an isotopicallyheavy solution. In addition, some of the silica released into solution by weathering can be absorbedon the surface of oxides and hydroxides in soils such as ferrihydrite and goethite. Delstanche etal. (2009) experimentally determined fractionation factors for adsorption of Si on ferrihydrite as ∆ 29 Si ferrisolu.≈ -0.81‰ and ∆ 29 Si geoth.-solu. ≈ -0.54‰. Assuming mass-dependent fractionation these imply 30 Si fractionationfactors of ∆ 30 Si ferri-solu. ≈ -1.59‰ and ∆ 30 Si geoth.-solu. ≈ -1.06‰. This adsorption drives dissolved silicafurther toward isotopically heavy compositions. The solubility of silica is quite limited; concentrationsin rivers are typically less than 10 ppm. Consequently, isotopic fractionation between dissolvedsilica and solid phases has a smaller effect on the isotopic composition of solid phases than the solution.In addition to being the key ingredient in silicate rocks and minerals, silicon is also extensively bioutilized.Terrestrial plants take-up silicic acid from the soil solution and incorporate it in various tissues,where it appears to increase rigidity, increase photosynthetic efficiency, limit loss of water byevapotranspiration, and increase the resistance to pathogens and grazing by herbivores, including insects.The ‘phytoliths’ formed in this process consist of hydrated opaline silica and vary widely in siliconisotopic composition. Ding et al. (2009) suggest the latter is due to Rayleigh fractionation duringprecipitation of the phytoliths from plant fluids with an apparent fractionation factor of ∆ 30 Si phyto-solu. ≈+2‰. This follows a fractionation during uptake of H 4 SiO 4 from the soil solution by roots of ∆ 30 Si roots-soil≈ -1.2‰. Thus silica utilization by plants drives the soil solution towards heavier isotopic compositions.In view of the fractionations during weathering and uptake by the terrestrial biota, it is not surprisingto find that rivers are isotopically heavy, with δ 30 Si ranging from -0.1‰ to +3.4‰ and averaging about+0.8‰ (De la Rocha et al., 1997; Georg et al., 2006; Ding et al., 2011). Isotopic compositions vary notonly between different rivers, but also over time in individual rivers. Georg et al. (2006) found thatδ 30 Si correlated positively with dissolved Si concentration and inversely with discharge and base cationflux. They suggest that the higher δ 30 Si are associated with active clay mineral formation during slowseepage of water through soils and low river discharge.Dissolved silica reaching the oceans is extensively bio-utilized and can be bio-limiting. Marine organismsutilizing silica include sponges and planktonic protists such as diatoms, silicoflagellates, and radiolarians.Of these, sponges appear to fractionate silica the most. De La Rocha (2003) found that δ 30 Si inmodern sponge spicules range from -1.2‰ to -3.7‰ and fractionation factors ∆ 30 Si sponge-sw averaged-3.8±0.8‰. Diatoms, which account for some 75% of primary productivity in the oceans, are far moreimportant in the marine silica cycle. These organisms live in the surface waters and build tests (orshells) of opaline silica. As a consequence, dissolved silica is depleted in the surface waters (Figure11.23). As their remains sink, the tests tend to redissolve and consequently deep waters are enriched indissolved silica. As we noted above, experiments suggest a fractionation factor, i.e., ∆ 30 Si opal-dissolv. , ofabout -1.1‰ during formation of diatom tests, and as a consequence surface waters are typically enrichedin 30 Si. Curiously, Demerest et al. (2009) found that the fractionation during partial dissolution ofdiatoms tests was just the opposite: the solution became isotopically lighter and the residual tests isotopicallyheavier with a ∆ 30 Si opal-dissolv. ≈ +0.55‰. Thus in both precipitation and dissolution of diatomtests, the lighter isotope reacts more readily (see Problem 11.4).Because δ 30 Si is oceans is tightly coupled with biological productivity and hence the carbon cycle,there is much interest in using silicon isotopes in understanding the modern silica cycle and using δ 30 Siin siliceous biogenic sediments to reconstruct productivity variations in the ancient oceans. To date,only a few such studies have been carried out, and interpretation of these variations remains somewhatequivocal. Improved understanding of the silica cycle in the modern ocean is needed before δ 30 Si can beused as a paleo-oceanographic proxy.368 1/9/13

Isotope GeochemistryW, M. White Chapter 11Figure 11.23. Variation of δ 30 Si and dissolvedsilica concentration with depth inthe equatorial Pacific. Data from Beucher etal. (2008).The silicon isotopic composition of seawaterthrough time has been controlled by (1) the isotopiccomposition of the sources of dissolved Si and (2)their relative fluxes and (3) fractionations occurringduring removal of Si from seawater. The principalfluxes are (a) weathering of continental (i.e., rivers),(b) submarine hydrothermal vents and (c) dissolvedSi diffusing out of sediments. Variations in the Siisotopic composition of seawater are recorded incherts, which are ubiquitous throughout thesedimentary record. Modern cherts are derivedprimarily from biogenic opal produced by diatoms,which became important in the sedimentary recordin the Mesozoic, and radiolarians, which first appearedin the Cambrian. Such silica-utilizing organismswere absent in the Precambrian (except forsponges in the latest Proterozoic), yet cherts arefound throughout the Precambrian. ManyPrecambrian cherts appear to have formedsecondarily through reaction of sedimentary andigneous rocks with Si-rich diagenetic fluids and donot provide a record of δ 30 Si in seawater. OtherPrecambrian cherts, however, likely formed throughdirect abiogenic precipitation from H 4 SiO 4 -saturatedseawater and/or hydrothermal fluids (in the absenceof silica-secreting organisms, dissolved silicaconcentrations in Precambrian oceans were likelymuch higher). Chakrabarti et al. (2012) found thatbanded iron formations (BIFs), which typicallyconsists of alternating Fe-rich and SiO 2 -rich layers,have lighter Si isotopic compositions than non-BIFPrecambrian cherts, which they argue is due to agreater hydrothermal component in BIF cherts. They found that δ 30 Si of Archean cherts progressivelyincreased with time, consistent with increasing input of dissolved Si from weathering of growing continentsand decreasing hydrothermal activity over this period. Submarine hydrothermal activity is associatedwith mid-ocean ridge and island-arc volcanism and a decrease with time is, of course, what weexpect for an Earth that is slowly cooling. Maximum δ 30 Si occurred at around 1.5 Ga in the Mesoproterozoic,after which δ 30 Si appears to decrease again. The cause of the latter decrease in not yet fullyunderstood, but this study makes clear that understanding how δ 30 Si has varied through time will helpus understand the evolution of the Earth.11.9 CHLORINE ISOTOPESChlorine has two isotopes 35 Cl and 37 Cl whose abundances are 75.76% and 24.24%, respectivelyCousey et al. 2011). It is most commonly in the -1 valance state and strongly electropositive, formingpredominantly ionic bonds, but in the rare circumstance of strongly oxidizing conditions it can havevalances up to +7. Chlorine is relatively volatile, and has a strong propensity to dissolve in water; consequentlymuch of the Earth’s inventory is in the oceans. Since the oceans are a large and isotopicallyuniform reservoir of chlorine (Godon et al., 2004), isotope ratios are reported as δ 37 Cl relative to seawaterchloride (formally called Standard Mean Ocean Chloride or SMOC with ratios denoted as369 1/9/13

Isotope GeochemistryW, M. White Chapter 11δ 37 Cl SMOC ), whose 37 Cl/ 35 is 0.319627 (Coplen et al., 2002). NIST-SRM 975 is the commonly used referencestandard, whose isotopic composition is73 Cl/ 35 Cl = 0.31977 (δ 37 Cl SMOC = +0.52‰) * .Relatively few Cl isotopic analyses of meteoriteshave been reported. Sharp et al.(2007) reported δ 37 Cl of +1.21‰ in Orgueil(CV1), +0.46‰ in Murchison (CM2) and -0.38‰ in Allende (CV3); components ofmeteorites such as water-soluble extractsand sodalite (Na 8 Al 6 Si 6 O 24 C l2 ) show greatervariability. Because the oceans andevaporites, which both have δ 37 Cl of ~0‰,likely contain more than 80% and possiblymore than 90% of the Earth’s chlorine inventory,the δ 37 Cl of the Earth is probablyclose to 0‰. Sharp et al. (2010) found thatδ 37 Cl in lunar materials ranged from -0.7‰Figure 11.24. Chlorine isotope variations in terrestrialmaterials and meteorites.to +24‰. They argued that both thepositive value and the large spread resultedfrom fractionation during volatilization andloss of metal chlorides during eruption ofthe basalts. That in turn, they suggested,indicated the Moon is hydrogen poorbecause formation of magmatic HCl lessensthe fractionation during degassing in terrestrialbasalts.Schauble et al. (2003) theoretically calculatedfactors for chlorine. They found (notsurprisingly) that the largest fractionationoccurred between chlorine of different oxidationstates. Fractionation between chlorides,chlorate (ClO 2 ), and perchlorate (ClO 4–) are as great as 27‰ and 73‰ at 298K, with37 Cl concentrating in the oxidized forms;however, naturally occurring chlorine inthese oxidized forms is extremely rare andplays essentially no role in the natural chlorinecycle. Among chlorides, they predictedthat 37 Cl will preferentially partition intoorganic molecules (by 5 to 9‰ at 295K) andinto salts and silicates where it is bound todivalent metals (e.g., FeCl 2 ) in preference tomonovalent ones (such as NaCl) by 2 to 3‰at 298K. 37 Cl should also concentrate in silicatesrelative to brines by 2 to 3‰ at surfacetemperature. They also calculated ∆ Cl2 -HCl =* The supply of this standard has been exhausted and it has been superseded by NIST-SRM 975a, whose 37 Cl/ 35 Cl =0.31970.370 1/9/13

Isotope GeochemistryW, M. White Chapter 11variability than high temperature ones, although those with the highest temperatures (>400˚ C) havemore uniform δ 37 Cl (1.0±1.3‰). Since the fractionations between HCl gas and Cl - solutions should be

Isotope GeochemistryW, M. White Chapter 11tremely light δ 37 Cl and serpentinite muds and clasts can have δ 37 Cl ranging from -0.22 to 1.61‰ (Barneset al., 2008). Subduction-related volcanics also exhibit a large range in δ 37 Cl: -2.6 to +2.4‰. Nevertheless,the combined range of δ 37 Cl in MORB and OIB exceeds all of these variations. Understanding themwill undoubted lead to important new insights into the origin of mantle reservoirs.REFERENCES AND SUGGESTIONS FOR FURTHER READINGAlexander, B., J. Savarino, N. Barkov, R. J. Delmas and M. H. Thiemens, Climate driven changes in theoxidation pathways of atmospheric sulfur, Geophysical Research Letters, 29: 301-304, 2003.Amini, M., Eisenhauer, A., Böhm, F., Fietzke, J., Bach, W., Garbe-Schönberg, D., Rosner, M., Bock, B.,Lackschewitz, K.S., Hauff, F., 2008. Calcium isotope (δ 44/40 Ca) fractionation along hydrothermalpathways, Logatchev field (Mid-Atlantic Ridge, 14˚45'N). Geochimica et Cosmochimica Acta, 72, 4107-4122.Anbar, A. D. 2004. Molybdenum stable isotopes: observations, interpretations, and directions. In: Johnson,C. M., Beard, B.L. & Albarède, F. (eds.) Geochemistry of Non-traditional Stable Isotopes. Washington:MSA.Anbar, A. D. and O. Rouxel, 2007. Metal stable isotopes in paleoceanography, Annual Reviews of Earthand Planetary Sciences, 35: 717-746, doi:10.1146/annurev.earth.34.031405.125029.Andersen, M. B., Vance, D., Archer, C., Anderson, R. F., Ellwood, M. J. & Allen, C. S. 2011. The Znabundance and isotopic composition of diatom frustules, a proxy for Zn availability in ocean surfaceseawater. Earth and Planetary Science Letters, 301, 137-145.Armytage, R.M.G., Georg, R.B., Savage, P.S., Williams, H.M., Halliday, A.N., 2011. Silicon isotopes inmeteorites and planetary core formation. Geochimica et Cosmochimica Acta, 75, 3662-3676, doi:10.1016/j.gca.2011.03.044.Armytage, R.M.G., Georg, R.B., Williams, H.M., Halliday, A.N., 2012. Silicon isotopes in lunar rocks:Implications for the Moon’s formation and the early history of the Earth. Geochimica et CosmochimicaAct,a 77, 504-514, doi: 10.1016/j.gca.2011.10.032.Asael, D., Matthews, A., Oszczepalski, S., Bar-Matthews, M. & Halicz, L. 2009. Fluid speciation controlsof low temperature copper isotope fractionation applied to the Kupferschiefer and Timna ore deposits.Chemical Geology, 262, 147-158.Barling, J., Arnold, G. L. & Anbar, A. D. 2001. Natural mass-dependent variations in the isotopic compositionof molybdenum. Earth and Planetary Science Letters, 193, 447-457.Barnes, J. D., Sharp, Z. D. & Fischer, T. P. 2008. Chlorine isotope variations across the Izu-Bonin-Mariana arc. Geology, 36, 883-886.Barnes, J. D., Paulick, H., Sharp, Z. D., Bach, W. & Beaudoin, G. 2009. Stable isotope (δ1 8 O, δD, δ 37 Cl)evidence for multiple fluid histories in mid-Atlantic abyssal peridotites (ODP Leg 209). Lithos, 110, 83-94, doi: 10.1016/j.lithos.2008.12.004.Becker, H. & Walker, R. J. 2003. Efficient mixing of the solar nebula from uniform Mo isotopic compositionof meteorites. Nature, 425, 152-155.Ben Othman, D., Luck, J. M., Bodinier, J. L., Arndt, N. T. & Albarède, F. 2006. Cu–Zn isotopic variationsin the Earth's mantle. Geochimica et Cosmochimica Acta, 70, A46.Bermin, J. 2006. Determination of the isotopic composition of Cu and Zn in seawater. PhD dissertation,Univ. of London.Bermin, J., Vance, D., Archer, C. & Statham, P. J. 2006. The determination of the isotopic composition ofCu and Zn in seawater. Chemical Geology, 226, 280-297.Beucher, C.P., Brzezinski, M.A., Jones, J.L., 2008. Sources and biological fractionation of Silicon isotopesin the Eastern Equatorial Pacific. Geochimica et Cosmochimica Acta 72, 3063-3073.Bishop, M. C., Moynier, F., Weinstein, C., Fraboulet, J.-G., Wang, K. & Foriel, J. 2012. The Cu isotopiccomposition of iron meteorites. Meteoritics & Planetary Science, 47, 268-276.373 1/9/13

Isotope GeochemistryW, M. White Chapter 11Black, J. R., Kavner, A. & Schauble, E. A. 2011. Calculation of equilibrium stable isotope partition functionratios for aqueous zinc complexes and metallic zinc. Geochimica et Cosmochimica Acta, 75, 769-783.Böhm, F., Gussone, N., Eisenhauer, A., Dullo, W.-C., Reynaud, S., Paytan, A., 2006. Calcium isotopefractionation in modern scleractinian corals. Geochimica et Cosmochimica Acta 70, 4452-4462.Bonifacie, M., Jendrzejewski, N., Agrinier, P., Coleman, M., Pineau, F. & Javoy, M. 2007. Pyrohydrolysis-IRMSdetermination of silicate chlorine stable isotope compositions. Application to oceanic crustand meteorite samples. Chemical Geology, 242, 187-201.Bonifacie, M., Jendrzejewski, N., Agrinier, P., Humler, E., Coleman, M. & Javoy, M. 2008. The chlorineisotope composition of Earth's mantle. Science, 319, 1518-1520.Brucker, R. L. P., McManus, J., Severmann, S. & Berelson, W. M. 2009. Molybdenum behavior duringearly diagenesis: insights from Mo isotopes. Geochemistry Geophysics Geosystems, 10, Q06010, doi:10.1029/2008gc002180.Burkhardt, C., Kleine, T., Oberli, F., Pack, A., Bourdon, B. & Wieler, R. 2011. Molybdenum isotopeanomalies in meteorites: Constraints on solar nebula evolution and origin of the Earth. Earth andPlanetary Science Letters, 312, 390-400.Came, R. E., Eiler, J. M., Veizer, J., Azmy, K., Brand, U. & Weidman, C. R. 2007. Coupling of surfacetemperatures and atmospheric CO 2 concentrations during the Palaeozoic era. Nature, 449, 198-201.Canfield, D. E., 2005. The early history of atmospheric oxygen: Homage to Robert M. Garrels, AnnualReviews of Earth and Planetary Sciences, 33: 1-36, doi:10.1146/annurev.earth.33.092203.122711.Cenki-Tok, B., Chabaux, F., Lemarchand, D., Schmitt, A. D., Pierret, M. C., Viville, D., Bagard, M. L. &Stille, P. 2009. The impact of water–rock interaction and vegetation on calcium isotope fractionationin soil- and stream waters of a small, forested catchment (the Strengbach case). Geochimica et CosmochimicaActa, 73, 2215-2228.Cerling, T. E., Bowman, J. R. & O'Neil, J. R. 1988. An isotopic study of a fluvial-lacustrine sequence: ThePlio-Pleistocene koobi fora sequence, East Africa. Palaeogeography, Palaeoclimatology, Palaeoecology, 63,335-356.Chakrabarti, R., Jacobsen, S.B., 2010. Silicon isotopes in the inner Solar System: Implications for coreformation, solar nebular processes and partial melting. Geochimica et Cosmochimica Acta, 74, 6921-6933,doi: 10.1016/j.gca.2010.08.034.Chakrabarti, R., Knoll, A.H., Jacobsen, S.B., Fischer, W.W., 2012. Si isotope variability in Proterozoiccherts. Geochimica et Cosmochimica Acta, 91, 187-201, doi: 10.1016/j.gca.2012.05.025.Chan, L. H., J. M. Edmond, G. Thompson and K. Gillis. 1992. Lithium isotopic composition of submarinebasalts: implications for the lithium cycle of the oceans. Earth and Planetary Science Letters, 108:151-160.Chan, L.-H. and F. A. Frey, Lithium isotope goechemistry of the Hawaiian plume: results from the HawaiiScientific Drilling Project and Koolau Volcano, Geochemistry Geophysics Geosystems, 4: doi:10.1029/2002GC000365, 2003.Chan, L.-H. and J. M. Edmond. 1988. Variation of lithium isotope composition in the marine environment:a preliminary report. Geochimica et Cosmochimica Acta 52: 1711-1717.Chaussidon, M. and A. Jambon. 1994. Boron content and isotopic composition of oceanic basalts: geochemicaland cosmochemical implications. Earth and Planetary Science Letters, 121: 277-291.Chaussidon, M. and B. Marty. 1995. Primitive boron isotope composition of the mantle. Science. 269:383-266.Chaussidon, M. and F. Albarède. 1992. Secular boron isotope variations in the continental crust: an ionmicroprobe study. Earth and Planetary Science Letters, 108: 229-241.Chu, N.-C., Henderson, G. M., Belshaw, N. S. & Hedges, R. E. M. 2006. Establishing the potential of Caisotopes as proxy for consumption of dairy products. Applied Geochemistry, 21, 1656-1667.374 1/9/13

Isotope GeochemistryW, M. White Chapter 11Cloquet, C., Carignan, J., Lehmann, M. & Vanhaecke, F. 2008. Variation in the isotopic composition ofzinc in the natural environment and the use of zinc isotopes in biogeosciences: a review. Analyticaland Bioanalytical Chemistry, 390, 451-463.Coplen, T. B., Böhlke, J. K., Bièvre, P. D., Ding, T., Holden, N. E., Hopple, J. A., Krouse, H. R., Lamberty,A., Peiser, H. S., Revesz, K., Rieder, S. E., Rosman, K. J. R., Roth, E., Taylor, P. D. P., R. D. Vocke, J. &Xiao, Y. K. 2002. Isotope-abundance variations of selected elements (IUPAC Technical Report). Pureand Applied Chemistry, 74, 1987-2017, doi:0.1351/pac200274101987.Coursey, J. S., Schwab, D. J., Tsai, J. J. & Dragoset, R. A. 2009. Atomic weights and isotopic compositionswith relative atomic masses [Online]. Gaithersburg, MD: NIST Physical Measurement Laboratory.Available: http://www.nist.gov/pml/data/comp.cfm 2012].Craddock, P. R. & Dauphas, N. 2011. Iron Isotopic Compositions of Geological Reference Materials andChondrites. Geostandards and Geoanalytical Research, 35, 101-123.Czaja, A. D., Johnson, C. M., Roden, E. E., Beard, B. L., Voegelin, A. R., Nägler, T. F., Beukes, N. J. &Wille, M. 2012. Evidence for free oxygen in the Neoarchean ocean based on coupled iron–molybdenum isotope fractionation. Geochimica et Cosmochimica Acta, 86, 118-137.Dahl, T. W., Canfield, D. E., Rosing, M. T., Frei, R. E., Gordon, G. W., Knoll, A. H. & Anbar, A. D. 2011.Molybdenum evidence for expansive sulfidic water masses in ~750 Ma oceans. Earth and PlanetaryScience Letters, 311, 264-274.Dahl, T. W., Hammarlund, E. U., Anbar, A. D., Bond, D. P. G., Gill, B. C., Gordon, G. W., Knoll, A. H.,Nielsen, A. T., Schovsbo, N. H. & Canfield, D. E. 2010. Devonian rise in atmospheric oxygen correlatedto the radiations of terrestrial plants and large predatory fish. Proceedings of the National Academyof Sciences, 107, 17911-17915.De La Rocha, C.L., 2003. Silicon isotope fractionation by marine sponges and the reconstruction of thesilicon isotope composition of ancient deep water. Geology 31, 423-426.De La Rocha, C.L., Brzezinski, M.A., DeNiro, M.J., 1997. Fractionation of silicon isotopes by marine diatomsduring biogenic silica formation. Geochimica et Cosmochimica Acta 61, 5051-5056.Demarest, M.S., Brzezinski, M.A., Beucher, C.P., 2009. Fractionation of silicon isotopes during biogenicsilica dissolution. Geochimica et Cosmochimica Acta 73, 5572-5583.DePaolo, D. J. 2004. Calcium isotopic variations produced by biological, kinetic, radiogenic, and nucleosyntheticprocesses. In: JOHNSON, C. M., BEARD, B. L. & ALBARÈDE, F. (eds.) Geochemistry of Non-Traditional Stable Isotopes. Washington, DC: Mineralogical Society of America.Ding, T.P., Gao, J.F., Tian, S.H., Wang, H.B., Li, M., 2011. Silicon isotopic composition of dissolved siliconand suspended particulate matter in the Yellow River, China, with implications for the globalsilicon cycle. Geochimica et Cosmochimica Acta 75, 6672-6689.Ding, T.P., Zhou, J.X., Wan, D.F., Chen, Z.Y., Wang, C.Y., Zhang, F., 2008. Silicon isotope fractionationin bamboo and its significance to the biogeochemical cycle of silicon. Geochimica et Cosmochimica Acta72, 1381-1395.Duan, Y., Anbar, A. D., Arnold, G. L., Lyons, T. W., Gordon, G. W. & Kendall, B. 2010. Molybdenumisotope evidence for mild environmental oxygenation before the Great Oxidation Event. Geochimicaet Cosmochimica Acta, 74, 6655-6668.Eagle, R. A., Schauble, E. A., Tripati, A. K., Tütken, T., Hulbert, R. C. & Eiler, J. M. 2010. Body temperaturesof modern and extinct vertebrates from 13 C- 18 O bond abundances in bioapatite. Proceedings of theNational Academy of Sciences, 107, 10377-10382, doi:10.1073/pnas.0911115107.Eagle, R. A., Tütken, T., Martin, T. S., Tripati, A. K., Fricke, H. C., Connely, M., Cifelli, R. L. & Eiler, J. M.2011. Dinosaur Body Temperatures Determined from Isotopic ( 13 C- 18 O) Ordering in Fossil Biominerals.Science, doi:10.1126/science.1206196.Eastoe, C. J., Peryt, T. M., Petrychenko, O. Y. & Geisler-Cussey, D. 2007. Stable chlorine isotopes inPhanerozoic evaporites. Applied Geochemistry, 22, 575-588, doi: 10.1016/j.apgeochem.2006.12.012.375 1/9/13

Isotope GeochemistryW, M. White Chapter 11Eggenkamp, H. G. M., Kreulen, R. & Koster Van Groos, A. F. 1995. Chlorine stable isotope fractionationin evaporites. Geochimica et Cosmochimica Acta, 59, 5169-5175.Elliott, T., A. Jeffcoate and C. Bouman, The terrestrial Li isotope cycle: light-weight constraints on mantleconvection, Earth and Planetary Science Letters 220: 231-245, 2004.Elliott, T., A. Thomas, A. Jeffcoate and Y. Niu, Lithium isotope evidence for subduction-enriched mantlein the source of mid-ocean-ridge basalts, Nature, 443:565-568, 2006.Farkaš, J., Böhm, F., Wallmann, K., Blenkinsop, J., Eisenhauer, A., van Geldern, R., Munnecke, A., Voigt,S., Veizer, J., 2007. Calcium isotope record of Phanerozoic oceans: Implications for chemical evolutionof seawater and its causative mechanisms. Geochimica et Cosmochimica Acta 71, 5117-5134.Farquhar, J. and B. A. Wing, Multiple sulfur isotopes and the evolution of atmospheric oxygen, Earthand Planetary Science Letters, 213: 1-13, 2003.Farquhar, J., B. A. Wing, K. D. McKeegan, J. W. Harris, P. Cartigny and M. Thiemens, Massindependentfractionation sulfur of inclusions in diamond and sulfur recycling on early Earth, Science,298: 2369-2372, 2002.Farquhar, J., H. Bao and M. Thiemens, Atmospheric influence of Earth's earliest sulfur cycle, Science,289: 756-758, 2000.Fernandez, A. & Borrok, D. M. 2009. Fractionation of Cu, Fe, and Zn isotopes during the oxidativeweathering of sulfide-rich rocks. Chemical Geology, 264, 1-12.Fitoussi, C., Bourdon, B., 2012. Silicon Isotope Evidence Against an Enstatite Chondrite Earth. Science335, 1477-1480, doi: 10.1126/science.1219509.Fitoussi, C., Bourdon, B., Kleine, T., Oberli, F., Reynolds, B.C., 2009. Si isotope systematics of meteoritesand terrestrial peridotites: implications for Mg/Si fractionation in the solar nebula and for Si in theEarth's core. Earth and Planetary Science Letters, 287, 77-85, doi: 10.1016/j.epsl.2009.07.038.Foster, G. L., Pogge von Strandmann, P. A. E. & Rae, J. W. B. 2010. Boron and magnesium isotopic compositionof seawater. Geochem. Geophys. Geosyst., 11: Q08015, doi: 10.1029/2010GC003201.Foster, G. L., Seawater pH, pCO 2 and [CO 2 -3 ] variations in the Caribbean Sea over the last 130kyr: A boronisotope and B/Ca study of planktic foraminifera, Earth and Planetary Science Letters, 271: 254-266,10.1016/j.epsl.2008.04.015 2008.Fujii, T., Moynier, F., Telouk, P. & Abe, M. 2010. Experimental and Theoretical Investigation of IsotopeFractionation of Zinc between Aqua, Chloro, and Macrocyclic Complexes. The Journal of PhysicalChemistry A, 114, 2543-2552.Gao, Y. Q. and R. A. Marcus, Strange and unconventional isotope effects in ozone formation, Science,293:259-263, 2001.Georg, R. B., Reynolds, B. C., Frank, M. & Halliday, A. N. 2006. Mechanisms controlling the silicon isotopiccompositions of river waters. Earth and Planetary Science Letters, 249, 290-306, doi:10.1016/j.epsl.2006.07.006.Godon, A., Jendrzejewski, N., Eggenkamp, H. G. M., Banks, D. A., Ader, M., Coleman, M. L. & Pineau,F. 2004. A cross-calibration of chlorine isotopic measurements and suitability of seawater as the internationalreference material. Chemical Geology, 207, 1-12.Gussone, N. & Filipsson, H. L. 2010. Calcium isotope ratios in calcitic tests of benthic foraminifers. Earthand Planetary Science Letters, 290, 108-117, doi: 10.1016/j.epsl.2009.12.010.Gussone, N., Böhm, F., Eisenhauer, A., Dietzel, M., Heuser, A., Teichert, B.M.A., Reitner, J., Wörheide,G., Dullo, W.-C., 2005. Calcium isotope fractionation in calcite and aragonite. Geochimica et CosmochimicaActa 69, 4485-4494, doi: 10.1016/j.gca.2005.06.003.Gussone, N., Eisenhauer, A., Heuser, A., Dietzel, M., Bock, B., Böhm, F., Spero, H. J., Lea, D. W., Bijma,J. & Nägler, T. F. 2003. Model for kinetic effects on calcium isotope fractionation (δ 44 Ca) in inorganicaragonite and cultured planktonic foraminifera. Geochimica et Cosmochimica Acta, 67, 1375-1382, doi:10.1016/s0016-7037(02)01296-6.376 1/9/13

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Isotope GeochemistryW, M. White Chapter 11Javoy, M., Kaminski, E., Guyot, F., Andrault, D., Sanloup, C., Moreira, M., Labrosse, S., Jambon, A.,Agrinier, P., Davaille, A. & Jaupart, C. 2010. The chemical composition of the Earth: Enstatite chondritemodels. Earth and Planetary Science Letters, 293, 259-268.John, S. G., Geis, R. W., Saito, M. A. & Boyle, E. A. 2007. Zinc isotope fractionation during high-affinityand low-affinity zinc transport by the marine diatom Thalassiosira oceanica. Limnology and Oceanography,56, 2710–2714.John, S. G., Rouxel, O. J., Craddock, P. R., Engwall, A. M. & Boyle, E. A. 2008. Zinc stable isotopes inseafloor hydrothermal vent fluids and chimneys. Earth and Planetary Science Letters, 269, 17-28.John, T., Layne, G. D., Haase, K. M. & Barnes, J. D. 2010. Chlorine isotope evidence for crustal recyclinginto the Earth's mantle. Earth and Planetary Science Letters, 298, 175-182.Johnson, C. M., B. L. Beard and E. E. Roden, The iron isotope fingerprints of redox and biogeochemicalcycling in modern and ancient Earth, Annual Reviews of Earth and Planetary Sciences, 36: 457-493, doi:doi:10.1146/annurev.earth.36.031207.124139, 2008.Johnson, C. M., Beard, B. L. & Albarede, F. 2004. Geochemistry of Non-Traditional Stable Isotopes, Washington,Mineralogical Society of America.Johnson, D. G., K. W. Jucks, W. A. Traub and K. V. Chance, 2001. Isotopic composition of stratosphericozone, J. Geohys. Res., 105:9025-9031.Kasting, J. F. and D. Catling, Evolution of a Habitable Planet, Annual Reviews of Astronony and Astrophysics,41:429-463, 2003.Kendall, B., Creaser, R. A., Gordon, G. W. & Anbar, A. D. 2009. Re-Os and Mo isotope systematics ofblack shales from the Middle Proterozoic Velkerri and Wollogorang Formations, McArthur Basin,northern Australia. Geochimica et Cosmochimica Acta, 73, 2534-2558.Kısakürek, B., Eisenhauer, A., Böhm, F., Hathorne, E. C. & Erez, J. 2011. Controls on calcium isotopefractionation in cultured planktic foraminifera, Globigerinoides ruber and Globigerinella siphonifera.Geochimica et Cosmochimica Acta, 75, 427-443.Klochko, K., A. J. Kaufman, W. Yao, R. H. Byrne and J. A. Tossell, 2006. Experimental measurement ofboron isotope fractionation in seawater, Earth and Planetary Science Letters, 248: 276-285, doi:10.1016/j.epsl.2006.05.034.Larson, P. B., Maher, K., Ramos, F. C., Chang, Z., Gaspar, M. & Meinert, L. D. 2003. Copper isotope ratiosin magmatic and hydrothermal ore-forming environments. Chemical Geology, 201, 337-350.Layne, G. D., Kent, A. J. R. & Bach, W. 2009. δ 37 Cl systematics of a backarc spreading system: The LauBasin. Geology, 37, 427-430, doi: 10.1130/g25520a.1.Li, W., Jackson, S. E., Pearson, N. J., Alard, O. & Chappell, B. W. 2009. The Cu isotopic signature ofgranites from the Lachlan Fold Belt, SE Australia. Chemical Geology, 258, 38-49.Liebscher, A., Barnes, J. & Sharp, Z. 2006. Chlorine isotope vapor–liquid fractionation during experimentalfluid-phase separation at 400˚C/23MPa to 450 ˚C/42MPa. Chemical Geology, 234, 340-345.Luck, J.-M., Othman, D. B. & Albarède, F. 2005. Zn and Cu isotopic variations in chondrites and ironmeteorites: Early solar nebula reservoirs and parent-body processes. Geochimica et Cosmochimica Acta,69, 5351-5363.Maréchal, C. N., Nicolas, E., Douchet, C. & Albarède, F. 2000. Abundance of zinc isotopes as a marinebiogeochemical tracer. Geochemistry Geophysics Geosystems 1, 1-15.Marèchal, C. N., Tèlouk, P. & Albarède, F. 1999. Precise analysis of copper and zinc isotopic compositionsby plasma-source mass spectrometry. Chemical Geology, 156, 251-273.Markl, G., Lahaye, Y. & Schwinn, G. 2006. Copper isotopes as monitors of redox processes in hydrothermalmineralization. Geochimica et Cosmochimica Acta, 70, 4215-4228.Marriott, C.S., Henderson, G.M., Belshaw, N.S., Tudhope, A.W., 2004. Temperature dependence of δ 7 Li,δ 44 Ca and Li/Ca during growth of calcium carbonate. Earth and Planetary Science Letters, 222, 615-624.378 1/9/13

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Isotope GeochemistryW, M. White Chapter 11Savage, P.S., Georg, R.B., Armytage, R.M.G., Williams, H.M., Halliday, A.N., 2010. Silicon isotope homogeneityin the mantle. Earth and Planetary Science Letters, 295, 139-146.Savage, P. S., Georg, R. B., Williams, H. M., Turner, S., Halliday, A. N. & Chappell, B. W. 2012. The siliconisotope composition of granites. Geochimica et Cosmochimica Acta, 92, 184-202, doi:10.1016/j.gca.2012.06.017.Schauble, E. A. 2011. First-principles estimates of equilibrium magnesium isotope fractionation in silicate,oxide, carbonate and hexaaquamagnesium(2+) crystals. Geochimica et Cosmochimica Acta, 75, 844-869, doi:10.1016/j.gca.2010.09.044.Schauble, E. A., Georg, R. B. & Halliday, A. N. 2007. Silicate metal fractionation of silicon isotopes athigh pressure and temperature. Eos Trans. AGU Fall Meet. Suppl., 88 (52), V42A-07.Schauble, E. A., Rossman, G. R. & Taylor Jr, H. P. 2003. Theoretical estimates of equilibrium chlorineisotopefractionations. Geochimica et Cosmochimica Acta, 67, 3267-3281, doi: 10.1016/s0016-7037(02)01375-3.Schauble, E.A., Georg, R.B., Halliday, A.N., 2007. Silicate metal fractionation of silicon isotopes at highpressure and temperature. Eos Trans. AGU Fall Meet. Suppl. 88 (52), V42A-07.Schwarcz, H. P., Agyei, E. K. & McMullen, C. C. 1969. Boron isotopic fractionation during clay adsorptionfrom sea-water. Earth and Planetary Science Letters, 6, 1-5,Seitz, H.-M., G. P. Brey, J. Zipfel, U. Ott, S. Weyer, S. Durali and S. Weinbruch, Lithium isotope compositionof ordinary and carbonaceous chondrites, and differentiated planetary bodies: Bulk solar systemand solar reservoirs, Earth and Planetary Science Letters, 260: 582-596, doi: 10.1016/j.epsl.2007.06.019, 2007.Seo, J. H., Lee, S. K. & Lee, I. 2007. Quantum chemical calculations of equilibrium copper (I) isotopefractionations in ore-forming fluids. Chemical Geology, 243, 225-237.Shahar, A., Hillgren, V.J., Young, E.D., Fei, Y., Macris, C.A., Deng, L., 2011. High-temperature Si isotopefractionation between iron metal and silicate. Geochimica et Cosmochimica Acta, 75, 7688-7697.Sharp, Z. D., Barnes, J. D., Brearley, A. J., Chaussidon, M., Fischer, T. P. & Kamenetsky, V. S. 2007. Chlorineisotope homogeneity of the mantle, crust and carbonaceous chondrites. Nature, 446, 1062-1065doi: 10.1038/nature05748.Sharp, Z. D., Barnes, J. D., Fischer, T. P. & Halick, M. 2010. An experimental determination of chlorineisotope fractionation in acid systems and applications to volcanic fumaroles. Geochimica et CosmochimicaActa, 74, 264-273, doi: 0.1016/j.gca.2009.09.032.Sharp, Z. D., Shearer, C. K., McKeegan, K. D., Barnes, J. D. & Wang, Y. Q. 2010. The chlorine isotopecomposition of the moon and implications for an anhydrous mantle. Science, 329, 1050-1053, doi:10.1126/science.1192606.Shen, B., Jacobsen, B., Lee, C.-T. A., Yin, Q.-Z., Morton, D. M. & Sleep, N. H. 2009. The Mg Isotopic Systematicsof Granitoids in Continental Arcs and Implications for the Role of Chemical Weathering inCrust Formation. Proceedings of the National Academy of Sciences, 106, 20652-20657.Siebert, C., Nägler, T. F., von Blanckenburg, F. & Kramers, J. D. 2003. Molybdenum isotope records as apotential new proxy for paleoceanography. Earth and Planetary Science Letters, 211, 159-171.Sime, N.G., De La Rocha, C.L., Galy, A., 2005. Negligible temperature dependence of calcium isotopefractionation in 12 species of planktonic foraminifera. Earth and Planetary Science Letters, 232, 51-66.Sime, N.G., De La Rocha, C.L., Tipper, E.T., Tripati, A., Galy, A., Bickle, M.J., 2007. Interpreting the Caisotope record of marine biogenic carbonates. Geochimica et Cosmochimica Acta, 71, 3979-3989.Simon, J. I. & DePaolo, D. J. 2010. Stable calcium isotopic composition of meteorites and rocky planets.Earth and Planetary Science Letters, 289, 457-466, doi:10.1016/j.epsl.2009.11.035.Simon, J.I., DePaolo, D.J., Moynier, F., 2009. Calcium Isotope Composition of Meteorites, Earth, andMars. The Astrophysical Journal, 702, 707.Skulan, J. & DePaolo, D. J. 1999. Calcium isotope fractionation between soft and mineralized tissues as amonitor of calcium use in vertebrates. Proceedings of the National Academy of Sciences, 96, 13709-13713.381 1/9/13

Isotope GeochemistryW, M. White Chapter 11Smith, H. J., A. J. Spivack, H. Staudigel and S. R. Hart, The boron isotopic composition of altered oceaniccrust, Chem. Geol., 126: 119-135, 1995.Sobolev, A.V., Hofmann, A.W., Sobolev, S.V., Nikogosian, I.K., 2005. An olivine-free mantle source ofHawaiian shield basalts. Nature 434, 590-597.Spivack, A. and J. M. Edmond. 1987. Boron isotope exchange between seawater and the oceanic crust.Geochimica et Cosmochimica Acta, 51: 1033-1044.Spivack, A. J., C.-F. You and H. J. Smith. 1993. Foraminiferal boron isotope ratios as a proxy for surfaceocean pH over the past 21 Myr. Nature. 363: 149-151.Telus, M., Dauphas, N., Moynier, F., Tissot, F. o. L. H., Teng, F.-Z., Nabelek, P. I., Craddock, P. R. &Groat, L. A. 2012. Iron, zinc, magnesium and uranium isotopic fractionation during continental crustdifferentiation: The tale from migmatites, granitoids, and pegmatites. Geochimica et Cosmochimica Acta,97, 247-265.Teng, F.-Z., Dauphas, N. & Helz, R. T. 2008. Iron Isotope Fractionation During Magmatic Differentiationin Kilauea Iki Lava Lake. Science, 320, 1620-1622, doi:10.1126/science.1157166.Teng, F.-Z., Dauphas, N., Helz, R. T., Gao, S. & Huang, S. 2011. Diffusion-driven magnesium and ironisotope fractionation in Hawaiian olivine. Earth and Planetary Science Letters, 308, 317-324, doi:10.1016/j.epsl.2011.06.003.Teng, F.-Z., McDonough, W. F., Rudnick, R. L. & Walker, R. J. 2006. Diffusion-driven extreme lithiumisotopic fractionation in country rocks of the Tin Mountain pegmatite. Earth and Planetary Science Letters,243, 701-710, doi:10.1016/j.epsl.2006.01.036.Teng, F.-Z., Li, W.-Y., Ke, S., Marty, B., Dauphas, N., Huang, S., Wu, F.-Y. & Pourmand, A. 2010. Magnesiumisotopic composition of the Earth and chondrites. Geochimica et Cosmochimica Acta, 74, 4150-4166, doi: 10.1016/j.gca.2010.04.019.Teng, F.-Z., Li, W.-Y., Ke, S., Marty, B., Dauphas, N., Huang, S., Wu, F.-Y. & Pourmand, A. 2010. Magnesiumisotopic composition of the Earth and chondrites. Geochimica et Cosmochimica Acta, 74, 4150-4166, doi:10.1016/j.gca.2010.04.019.Teng, F.-Z., Li, W.-Y., Rudnick, R. L. & Gardner, L. R. 2010. Contrasting lithium and magnesium isotopefractionation during continental weathering. Earth and Planetary Science Letters, 300, 63-71,doi:10.1016/j.epsl.2010.09.036.Teng, F.-Z., McDonough, W. F., Rudnick, R. L., Dalpe, C., Tomascak, P. B., Chappell, B. W. & Gao, S.2004. Lithium isotopic composition and concentration of the upper continental crust. Geochimica etCosmochimica Acta, 68, 4167-4178.Thiemens, M., History and Applications of Mass-Independent Isotope Effects, Annual Reviews of Earthand Planetary Sciences, 34:217-262, 2006.Tipper, E.T., Gaillardet, J., Galy, A., Louvat, P., Bickle, M.J., Capmas, F., 2010. Calcium isotope ratios inthe world's largest rivers: A constraint on the maximum imbalance of oceanic calcium fluxes. GlobalBiogeochemical Cycles, 24, GB3019, doi: 10.1029/2009GB003574.Tomascak, P. B. 2004. Developments in the understanding and application of lithium isotopes in theEarth and planetary sciences. In: JOHNSON, C. M., BEARD, B. L. & ALBAREDE, F. (eds.) Geochemistryof Non-Traditional Stable Isotopes. Washington: Mineralogical Society of America.Tomascak, P. B., Tera, F., Helz, R. T. & Walker, R. J. 1999. The absence of lithium isotope fractionationduring basalt differentiation: new measurements by multicollector sector ICP-MS. Geochimica et CosmochimicaActa, 63, 907-910, doi:10.1016/s0016-7037(98)00318-4.Tonarini, S., Leeman, W. P. & Leat, P. T. 2011. Subduction erosion of forearc mantle wedge implicatedin the genesis of the South Sandwich Island (SSI) arc: Evidence from boron isotope systematics. Earthand Planetary Science Letters, 301, 275-284, doi:10.1016/j.epsl.2010.11.008.Vance, D., Archer, C., Bermin, J., Perkins, J., Statham, P. J., Lohan, M. C., Ellwood, M. J. & Mills, R. A.2008. The copper isotope geochemistry of rivers and the oceans. Earth and Planetary Science Letters,274, 204-213.382 1/9/13

Isotope GeochemistryW, M. White Chapter 11Veizer, J., Ala, D., Azmy, K., Bruchschen, P., Buhl, D., Bruhn, F., Carden, G., Diener, A., Ebneth, S.,Godderis, Y., Jasper, T., Korte, C., Pawellek, F., Podlaha, O. G. & Strauss, H. 1999. 87 Sr/ 86 Sr, δ 13 C, andδ 18 O evolution of Phanerozoic seawater. Chemical Geology, 161, 59-88.Vengosh, A., Y. Kolodny, A. Starinsky, A. Chivas and M. McCulloch. 1991. Coprecipitation and isotopicfractionation of boron in modern biogenic carbonates. Geochimica et Cosmochimica Acta 55: 2901-2910.Vlastèlic, I., Koga, K., Chauvel, C., Jacques, G. & Telouk, P. 2009. Survival of lithium isotopic heterogeneitiesin the mantle supported by HIMU-lavas from Rurutu Island, Austral Chain. Earth and PlanetaryScience Letters, 286, 456-466, doi:10.1016/j.epsl.2009.07.013.Voegelin, A. R., Nägler, T. F., Beukes, N. J. & Lacassie, J. P. 2010. Molybdenum isotopes in late Archeancarbonate rocks: Implications for early Earth oxygenation. Precambrian Research, 182, 70-82.Voegelin, A. R., Nägler, T. F., Samankassou, E. & Villa, I. M. 2009. Molybdenum isotopic composition ofmodern and Carboniferous carbonates. Chemical Geology, 265, 488-498.Wiegand, B. A., Chadwick, O. A., Vitousek, P. M. & Wooden, J. L. 2005. Ca cycling and isotopic fluxesin forested ecosystems in Hawaii. Geophysical Research Letters, 32, L11404, doi:10.1029/2005gl022746.White, W. M. & Klein, E. 2013. Composition of the Oceanic Crust. In: RUDNICK, R. L. (ed.) Treatise onGeochemistry Volume 3. The Crust. 2 ed. Amsterdam: Elsevier.Wei, W., Kastner, M. & Spivack, A. 2008. Chlorine stable isotopes and halogen concentrations in convergentmargins with implications for the Cl isotopes cycle in the ocean. Earth and Planetary ScienceLetters, 266, 90-104.Weiss, D. J., Mason, T. F. D., Zhao, F. J., Kirk, G. J. D., Coles, B. J. & Horstwood, M. S. A. 2005. Isotopicdiscrimination of zinc in higher plants. New Phytologist, 165, 703-710.Weyer, S., Anbar, A. D., Brey, G. P., Münker, C., Mezger, K. & Woodland, A. B. 2005. Iron isotope fractionationduring planetary differentiation. Earth and Planetary Science Letters, 240, 251-264.Wiechert, U. & Halliday, A. N. 2007. Non-chondritic magnesium and the origins of the inner terrestrialplanets. Earth and Planetary Science Letters, 256, 360-371, doi: 10.1016/j.epsl.2007.01.007.Williams, H. M. & Archer, C. 2011. Copper stable isotopes as tracers of metal–sulphide segregation andfractional crystallisation processes on iron meteorite parent bodies. Geochimica et Cosmochimica Acta,75, 3166-3178.Williams, H. M., Peslier, A. H., McCammon, C., Halliday, A. N., Levasseur, S., Teutsch, N. & Burg, J. P.2005. Systematic iron isotope variations in mantle rocks and minerals: The effects of partial meltingand oxygen fugacity. Earth and Planetary Science Letters, 235, 435-452.You, C.-F. 1994. Comment on “Boron content and isotopic composition of oceanic basalts: geochemicaland cosmochemical implications” by M. Chaussidon and A. Jambon. Earth and Planetary Science Letters,128: 727-730.You, C. F., Spivack, A. J., Gieskes, J. M., Rosenbauer, R. & Bischoff, J. L. 1995. Experimental study of borongeochemistry: implications for fluid processes in subduction zones. Geochimica et CosmochimicaActa, 59, 2435-2442.Young, E. D. & Galy, A. 2004. The isotope geochemistry and cosmochemistry of magnesium. In: Johnson,C. M., Beard, B. L. & Albarède, F. (eds.) Geochemistry of Non-traditional Stable Isotopes. Washington,DC: MSA.Young, E. D., Tonui, E., Manning, C. E., Schauble, E. & Macris, C. A. 2009. Spinel–olivine magnesiumisotope thermometry in the mantle and implications for the Mg isotopic composition of Earth. Earthand Planetary Science Letters, 288, 524-533.Zeebe, R., Stable boron isotope fractionation between dissolved B(OH) 3 and B(OH) 4 - , Geochimica et CosmochimicaActa, 69:2753-2766, 2005.Ziegler, K., Young, E.D., Schauble, E.A., Wasson, J.T., 2010. Metal–silicate silicon isotope fractionationin enstatite meteorites and constraints on Earth's core formation. Earth and Planetary Science Letters,295, 487-496.383 1/9/13

Isotope GeochemistryW, M. White Chapter 11Problems1. The present ocean has a δ 98/95 Mo of +2.3‰ and that the input to the ocean is 90% from rivers (δ 98/95 Mo= +0.7‰) and 10% from hydrothermal fluid (δ 98/95 Mo = +0.8‰). Let’s assume that remove of Mofrom the oceans occurs only through oxic adsorption onto Mn-Fe crusts from seawater and authigenicFe-Mo-S deposition reducing continental margin. Assume the fractionation for oxic adsorption(∆ Oxic ) is -3.0‰ and that removal by sulfide precipitation under anoxic conditions in sediments(∆ Anoxic ) is -0.6‰, what fraction of the removal occurs through oxic adsorption?2. The following are constants for the polynomial function approximating fractionation factors (equation11.09) between the listed phase and Mg g given by Schuable (2011):A B CDolomite 1.667 × 10 14 -1.2954 × 10 10 2.1154 × 10 6Mg 2+ aq 2.3453 × 10 14 -1.9796 × 10 10 2.5007 × 10 6a. Calculate the fractionation dolomite – Mg 2+ fractionation factor at 15˚ and 25˚C.b. Assuming that rivers are the only source of Mg to seawater and that they have δ 26 Mg of -1.1‰and that hydrothermal activity and dolomite formation are the only sinks, and that seawater is insteady state with δ 26 Mg = -0.82‰. If there is no fractionation in hydrothermal removal, use thefractionation factor you calculated above for 20˚C to determine what fractionation of seawaterMg is removed by dolomite formation. What would the isotopic composition of this dolomite be?c. Using the fraction of Mg removal by dolomite formation you calculated in (b.), how would theδ 26 Mg of seawater change if the temperature increased from 15˚ to 25˚C?3. Calcium has 6 stable isotopes, more than any other element with atomic number under 40.a. Why?b. Why does 40 Ca constitute more than 96% of calcium?4. The fractionation factor for the precipitation of opal by diatoms is ∆ 30 Si opal-dissolv. ≈ -1.1‰, while that forthe dissolution of diatoms tests is ∆ 30 Si opal-dissolv. ≈ +0.55‰; in other words, 28 Si appears to go preferentiallyinto the reactant in both reactions. What does this suggests controls the fractionation? Justify youranswer.384 1/9/13