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2'y astrrafiomical values depend on data which are very difficult to interprets Urey gives a smaller value than Goldschmidto Sudi values are probably in error on the loir side since iron sulfide would be reduced by hydrogen at moderate teraperatures* i« s. the nelting point of iron and loner, and hence sulfur was * probably partly lost as Ix^drogen sulfide during the formation of the niat«»oz*iteso Since sulfur exists in the carbon c
26o The heavier rare gases^ Bie rare gases with the exception of helium are not observed in the sun because of Its low temperature and their lo^ abundanceo Neon ai^ argon have been observed in 0 typo stars and planetazy nebulae. The data are reviewed by IJnsftld (1948) and by Aller (1953) o Certainly the probable limits of error are very large because the observed lin^s are those of the ions sad it is difficult to estimate the conditions of excitation with sufficient accuracy to secure the abundances within better than a factor of 10 with certalntyo The ratios of the rare gases in the atmosphere are well known
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: 24 abundances, R, and column three
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 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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