Standard solar model: Interplay between the equation of state, the opacity and the determination of the initial helium content

Details Standard solar model: Interplay between the equation of state, the opacity and the determination of the initial helium content Standard solar model: Interplay between the equation of state, the opacity and the determination of the initial helium content

Dec 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...280..666c&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 280, no. 2, p. 666-674

Astronomy and Astrophysics

Astronomy

13

Equations Of State, Helium, Opacity, Solar Interior, Solar Oscillations, Stellar Evolution, Stellar Models, Abundance, Helioseismology, Solar Convection (Astronomy), Solar Neutrinos

Scientific paper

Solar models computed with the Geneva evolutionary code are presented. We examine the sensitivity of the structure of the solar model to the microphysics. The influence of the equation of state, of the opacity and of the mixture of heavy elements on the determination of the initial solar helium content is discussed. Our reference model calculated with the best available input physics, i.e. with the Mihalas-Hummer-Daeppen equation of state and the new radiative opacities from Iglesias et al (1992) and Kurucz (1991), has an initial helium abundance Y = 0.2779 in mass fraction. The radius at the base of the convective zone reported to the solar radius is equal to 0.718, in excellent agreement with helioseismic observations. The central temperature has a value of 15.56 x 106 K. The predicted total neutrino capture rates for the chlorine and gallium experiments are respectively equal to 7.49 and 127.5 SNUs and that confirms that the so-called 'neutrino problem' persists in spite of the recent improvements of the physics.

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