Solar Structure in terms of Gauss' Hypergeometric Function

Details Solar Structure in terms of Gauss' Hypergeometric Function Solar Structure in terms of Gauss' Hypergeometric Function

1995-02-05

arxiv.org/abs/astro-ph/9502022v1

Astrophys. Space Sci. 228:77-86,1995

Astronomy and Astrophysics

Astrophysics

Invited Paper (A.M.Mathai) at the Fourth UN/ESA Workshop on Basic Space Science, Cairo, Egypt, July 1994, 10 pages LaTeX,4 fig

Scientific paper

10.1007/BF00984968

Hydrostatic equilibrium and energy conservation determine the conditions in the gravitationally stabilized solar fusion reactor. We assume a matter density distribution varying non- linearly through the central region of the Sun. The analytic solutions of the differential equations of mass conservation, hydrostatic equilibrium, and energy conservation, together with the equation of state of the perfect gas and a nuclear energy generation rate $\epsilon=\epsilon_0\rho^nT^m$, are given in terms of Gauss' hypergeometric function. This model for the structure of the Sun gives the run of density, mass pressure, temperature, and nuclear energy generation through the central region of the Sun. Because of the assumption of a matter density distribution, the conditions of hydrostatic equilibrium and energy conservation are separated from the mode of energy transport in the Sun.

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