The Solar Light-Element Abundances and Primeval Helium

Details The Solar Light-Element Abundances and Primeval Helium The Solar Light-Element Abundances and Primeval Helium

Aug 1970

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1970saosr.323.....m&link_type=abstract

SAO Special Report #323 (1970)

Computer Science

3

Scientific paper

From a comparison of recent determinations of photospheric element abundances with solar cosmic-ray measurements, the abundances of helium, carbon, nitrogen, oxygen, neon, magnesium, silicon, and sulphur in the solar surface are determined within a probable error of 12%. The abundance of iron is also determined this way, but the resulting value may be in error by a factor of 2. The abundance of helium is found to be lower than the usually accepted 10% (i.e., Y= 0.28); it is 5.6% (i.e., Ysun = 0.188 +/- 0.020). Using a simple model for the exchange of material between stars and the interstellar matter, we find that a reasonable value for the initial helium fraction is then YO≅ 0.133, considerably smaller than the values generally obtained from hot big-bang models.

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