View Document - OSTI

More documents

Recommendations

Info

49 maximum age of the elements. If some Pb^*-*7 was produced by the processes which produced the elementsJ, the age is less than this. If the age is 5.2 x lO-' years, that Is one half life of U^^5 earlier than the age of the meteorites, the abundances of the lead Isotopes become 0,0101, 0.0153, and 0.0600 for Pb 207, pb^O^^ and Pb^^^, respectively. The logarithms of these are 0.004-2, 0.177-2 and 0.778-2. Taking the mean of the logarithms for Pb and Pb^^° and subtracting that for Pb^'"^ gives 0.47 as the difference between the odd and even mass curves. This difference as we have drawn the curves is 0.20 and hence it would be necessai^y to lower Bi209 and the thallium points by about 0.27 in order to secure a smooth curve. The data of these elements is hardly sufficiently certain to exclude this possibility. However, the difference of 0,47 between the two curves is larger than the separation of our even and odd mass curves at any point above mass 120, Since the odd and even mass curves become closer together at high mass numberSj It seems likely that the elements were synthesized more than 5,2 X 10^ years ago. This estimate does not depend on the absolute values of the abundances of lead and uranium, but only on their ratios which are determined from the lead isotope ratios. If the Patterson data for Nuovo laredo meteorite were used the calculated age of the elements would be less. On the other handp from the absence of conspicuous amounts of Xe-^^^ and the known half life of I^^9 in meteorites, Suess and Brown (I951) conclude that
50 the elements were formed at least 3 x 109 years before the meteorites. We conclude that the elements of our solar system originated 5-0 t 0.2 x 10^ years ago.
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 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: 48 We adopt values for u235, u^^°
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
show all

View Document - OSTI

Create successful ePaper yourself

Delete template?

Save as template?