New Solar Models Including Helioseismological Constraints and Light-Element Depletion

O. Richard, S. Vauclair, C. Charbonnel, W. A. Dziembowski

Published 1996-01-24, updated 1996-03-02Version 2

We have computed new solar models using the same stellar evolution code as described in Charbonnel, Vauclair and Zahn (1992). This code, originating from Geneva, now includes the computation of element segregation for helium and 12 heavier isotopes. It may also include any type of mixing of the stellar gas, provided this mixing may be parametrized with an effective diffusion coefficient as a function of radius. Here we introduced rotation-induced mixing as prescribed by Zahn (1992). We present five solar models: the standard model; two models including pure element segregation; two models with both element segregation and rotation-induced mixing. The $u = {P \over \rho }$ function computed as a function of radius in these new solar models are compared to the helioseismological results obtained for the same function by Dziembowski et al (1994). Improving the physics of the models leads to a better consistency with helioseismology. In our best model, which includes both segregation and mixing, the relative difference in the $ u $ function between the model and the helioseismological results is smaller than 0.5 per cent at all radii except at the center and the surface. Meanwhile lithium is depleted by a factor 155 and beryllium by a factor 2.9, which is consistent with the observations. The bottom of the convective zone lies at a fractional radius of 0.716, consistent with helioseismology. The neutrino fluxes are not decreased in any of these models. The models including the computations of element segregation lead to a present surface helium abundance of: $ Y_{surf} $ between 0.248 and 0.258, which is in satisfactory agreement with the value derived from helioseismology.