Changes of solar luminosity and radius following secular perturbations in the convective envelope

Details Changes of solar luminosity and radius following secular perturbations in the convective envelope Changes of solar luminosity and radius following secular perturbations in the convective envelope

Mar 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...290..748e&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 290, March 15, 1985, p. 748-757.

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Computation

43

Convection, Long Term Effects, Radii, Solar Magnetic Field, Stellar Envelopes, Stellar Luminosity, Computational Astrophysics, Energy Transfer, Nonadiabatic Conditions, Solar Physics

Scientific paper

The effect on solar models of several types of slow, spherically symmetric perturbations, acting at various depths within the convective envelope, are calculated. Results are presented on perturbations of the efficiency of convective energy transport (alpha perturbations) and on changes in the nongas component of pressure (beta perturbations). The effects of magnetic fields concentrated near the interface between the radiative core and the convective envelope are explored. It is found that the response and relaxation diagnostics depend both on the type of perturbation and on the depth at which the perturbation is applied. In addition to the general depth dependence, model behavior is sensitive to the presence of major ionization zones near the perturbed layer. The time dependence of the solar model behavior is characterized by an initial hydrostatic reaction followed by a thermal readjustment on a time scale of about 100 years, and finally relaxation to a new thermal equilibrium on a Kelvin time scale.

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