Astronomy and Astrophysics – Astronomy
Scientific paper
Feb 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983prhe.work..117g&link_type=abstract
IN: ESO Workshop on Primordial Helium, Garching, West Germany, February 2, 3, 1983, Proceedings (A83-50030 24-90). Garching, Wes
Astronomy and Astrophysics
Astronomy
8
Abundance, Helium, Protostars, Solar Oscillations, Stellar Evolution, Stellar Models, Calibrating, Flux (Rate), Solar Neutrinos
Scientific paper
The theory of stellar evolution applied to the sun cannot alone determine the solar helium abundance. Only if the neutrino flux is taken into account can a formal calibration be carried out. But that procedure appears to give the wrong result. An astronomical argument for calibrating mixing-length theory, using a measure of chromospheric activity in lower main-sequence stars, suggests that the protosolar abundance by mass is about 0.25. More direct measurements, using five-minute high-degree oscillation frequencies to measure conditions in the upper regions of the convection zone, and five-minute low-degree oscillations to probe the radiative interior, corroborate this finding. A recent unpublished report of quadrupole g-mode frequencies is also consistent. It is difficult to assess the uncertainty in the estimated abundance, because there are systematic unexplained discrepancies between theory and observation. However, the spread in the various determinations, excluding that involving the neutrino flux, is less than 10 percent of the mean value.
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