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39 The analyses of meteorites carried out by Ida Noddack (1935) lead to values considerably different from those given by Minami for terrestrial sediments. The ratio of La to the heavier rare earth elements, such as Er, Yb, etc., is about 8 times larger in Minami»s values for the sediments than in those of Noddack*s for the meteorites. It seems difficult to believe that a fractionation of that order of magnitude could have occurred during the formation of the earth, and it seems more probable that one of the series of analytical data is considerably in error. Minami*3 values for the abundances of the rare earth elements relative to each other in terrestrial sediments have been tentatively assumed here to give a closer approximation to the truth than the value given by Noddack. Qoldschmidt (1937), Brown (1949) and Urey (1958) all used Noddack*s values and hence considerable differences between their tables and the present table occur. The abundance of the group as a whole relative to silicon has been chosen ai'bitrarlly so as to secure what appears to the writers to be a reasonable interpolation to the lower and higher mean abundances. Our values certainly lie within i^asonable limits of error of the data. Considerable concentration of the group has occurred in the more acidic rocks and hence a somewhat lower value for lanthanum
40 than that given by Noddack (1955) is Justified. The abundances are adjusted only slightly from Minami's values in order to secure smoother curves. Table 5 compares the obsejrved and selected values both normalized to our lanthanum value. TABLE 5 La cat/ Pr Nd Sm Eu Minami«s abundances 1.00 2.46 0.295 1»25 0.215 0.052 Our abundances 1.00 1.13 0.20 0.72 0.324 0.093 Qd Tb Dy Ho Er Tm Minami»s abundances 0.31 0.043 0.21 0.052 0.11 0.0084 Our abundances 0.34 0.048 0.28 0,059 0,l6 0.0159 Yb Lu Minami*8 abundances 0.12 0.032 Our abundances 0,11 0.025 The most serious disagreement occurs in the case of cerium. discrepancies are surely within the observational errors, but also the true curves may be less regular than we have drawn them. The abundance of hafnium was taken as A/ 1/110 that of zirconium, as discussed above, Rankama (1944, 1948} gives the maximum amount of tantalum in meteorites as 0.38 ppm^ equivalent to an atomic abundance of 0
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 and 34: 30o valueso This ratio is 300 hy we
Page 35 and 36: greater constancy in the copper dat
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: 3Bo meteorites. We have selected a
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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