Approximating the solar/stellar energy generation rate, luminosity gradient, and the hydrogen content

Details Approximating the solar/stellar energy generation rate, luminosity gradient, and the hydrogen content Approximating the solar/stellar energy generation rate, luminosity gradient, and the hydrogen content

Apr 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994ap%26ss.214...19d&link_type=abstract

Astrophysics and Space Science, Vol. 214, No. 1-2, Proceedings of the second United Nations/European Space Agency Workshop, Bogo

Astronomy and Astrophysics

Astrophysics

Radiative Transfer, Solar Energy, Solar Interior, Stellar Luminosity, Stellar Models, Energy Distribution, Hydrogen-Based Energy, Luminous Intensity, Proton-Proton Reactions, Radial Distribution

Scientific paper

In this paper we wish to develop an analytical technique for modeling the energy generation rate and the luminosity gradient for a one solar mass star like the Sun. Following the Motz-Doorish Variables (MDV) method for approximating the solar/stellar structure (Doorish, 1989) we derive dimensionless variables for the energy generation rate and luminosity which are used in an expansion equation (on the order of a simple general confluent hypergeometric function). Modeling the luminosity of the Sun is complicated due to the nature of the energy generation rate. For this reason, we attempt to first derive approximation of the energy generation rate. The resulting solutions bring about a model of the luminosity gradient and the corresponding energy generation rate for the proton-proton cycle. Also, we are able to derive, analytically, the hydrogen content from the center of the star to the surface using concepts derived from the energy generation rate.

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