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31 ratio, namely 2.2^ x 10^ by weight. With our nickel value this gives O085O for the palladium abundance. Qoldschmidt gave 2.5 for this value. Qoldschmidt*8 assumption of a higher proportion of metallic phase increased his value. Using 10 per cent of the metallic phase and neglecting the trollite phase, his value becomes 0.9 ppm which is only slightly larger than our selected value. The Ni-Au ratio is also given by the studies of Qoldberg et al and this fixes the position of gold relative to nickel. These two ratios are the most reliable that we have for fixing the position of our curves over the high mass range. The atmospheric ratio of krjrpton to xenon by atoms la 12.5 and the solar ratio must be this value or higher since krypton may have escaped more readily than xenon, as explained above. It has been most interesting that throughout our attempts to secure the adjustment of abundances consistent with all the evidence, we have never found it desirable to increase this ratio above the value of 12-5. Our abundances of krypton and xenon, 25,0 and 2,00 respectively are consistent with this ratio. Copper, Zinc, Gallium, Germanium, Arsenic, Krypton, Strontium, Ytterbium Within reasonable estimates of the errors in the reported abundances of elements from Pe to Zr, it is possible to secure a smooth curve for the odd mass elements of this region. The pairs of Isotopes of Cu, Qa, and Br define the slope at three points. The general position of the curve is fixed by the Br and Rb abundances. "Bie Cu content of meteorites varies within surprisingly large limits. Qoldschmidt after an extensive discussion of the best data which vary by factors of more than 10, selected an atomic abundance of 460. Preliminary unpublished data of Wllk Indicate
greater constancy in the copper data for chondritic meteorites. Our choice of 228 for the atomic abundance results from a consideration of his data. Zinc in meteorites is typically chalcophile and is concentrated in the sulfide phase. Qoldschmidt's selection of data would require zinc to be less abundant than copper, which would be a surprising result. Uns51d»s value based on three lines in the solar spectrum is more than ten times higher than Qoldschmidt's estimate of 36O for the atomic abundeuice. We use 486 in order to secure smooth abundance curves In this region. This value is surely within the errors of the analytical data. Qallium has been studied in the iron meteorites by QoldbeiTg, Uchiyama and Brown (I951) who found three groups of iron meteorites having quite distinctly different contents of gallitua, namely, 60, 20 and 2 ppm, respectively. 52 Ko satisfactory explanation of this variation has been given. These abundances are puzzling particularly since gallium is a rather electropositive element and is concentrated to some extent in the surface terrestrial rocks. It seems probable that gallium is present partly in the silicate phases as well. We use 14.6 for this to abundance, equivalent/^7 ppm, which makes scandium 3.3 times as abundant as gallium, thus meeting to some extent the observations of Russell regarding the relative abundances of these elements. It would be difficult to be certain that gallium should not be lower or scandium higher or both. The careful studies of Qoldschmidt and Peters (1933a) on the germanium content of meteorites gave a meaui of 79 ppm in their average of the silicate, trollite and metallic phases. The germanium (See insert page 32)
Page 1 and 2: 05" 9003'9 ,^ r.V- ou 15 -^ CBNTiJA
Page 3 and 4: DISCLAIMER Portions of this documen
Page 5 and 6: o which states that the elements wi
Page 7 and 8: inattention will be drawn to any ev
Page 9 and 10: 6 the proportions 10:1:2- The Nodda
Page 11 and 12: 8 Just in the case of these element
Page 13 and 14: 10 spectral lines on the temperatur
Page 15 and 16: 12 have studied the iron sulfide fr
Page 17 and 18: 14 the proportion of the three phas
Page 19 and 20: 16 by more than a factor of 10, e.g
Page 21 and 22: 18 million times smaller than that
Page 23 and 24: 20 as occurs at other points in the
Page 25 and 26: 22 220 ppm relative to silicon equa
Page 27 and 28: 24 abundances, R, and column three
Page 29 and 30: 26o The heavier rare gases^ Bie rar
Page 31 and 32: 28, the amount is very constant nea
Page 33: 30o valueso This ratio is 300 hy we
Page 37 and 38: 33 o mass curve we natst assun® ab
Page 39 and 40: 35. Noddack*s value of 1.86 for the
Page 41 and 42: 37 value. Undoubtedly a marked decr
Page 43 and 44: 3Bo meteorites. We have selected a
Page 45 and 46: 40 than that given by Noddack (1955
Page 47 and 48: 42 The average is secured by assumi
Page 49 and 50: 44 these data all appear to be doub
Page 51 and 52: 46 ppm are not presented with great
Page 53 and 54: 48 We adopt values for u235, u^^°
Page 55 and 56: 50 the elements were formed at leas
Page 57 and 58: i»2o for the sum of isobaric abund
Page 59 and 60: 5u« This means that the In^^^ in n
Page 61 and 62: :>6„ of the neutron excess number
Page 63 and 64: dance values fitting into the trend
Page 65 and 66: OUo 56 56 The hjalf life of m , whi
Page 67 and 68: TABLE II 6 Atomic Abundances of the
Page 69 and 70: TABLE II continued 3 45 Rh 1.3 3,5
Page 71 and 72: TABLE III Element A N I Log H H 1 H
Page 73 and 74: 21 22 23 24 25 26 27 28 29 Sc Ti V
Page 75 and 76: TABLE III Continued 5 37 Rb p- 37.
Page 77 and 78: 52 55 5^ 55 56 57 58 Te I Xe Cs Bn
Page 79 and 80: 67 Ho 68 Er 71 Lu 72 Hf 73 Ta 74 W
Page 81: TABLE III Continued 11 122 124 40 4
Page 86 and 87:
Blbliography-2 Pellenberger, Th.v.,
Page 88 and 89:
Pinson, W.H., Ahrens, L.H. and Fran
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