  The physical principles and the mathematical structure involved in deriving
an analytical representation of the internal structure of the sun are
discussed. For a two-parameter family of a non-linear matter density
distribution, the run of mass, pressure, temperature, and luminosity throughout
the sun are expressed in terms of Gauss' hypergeometric function. The system of
differential equations governing hydrostatic equilibrium and energy
conservation for the sun generates another field of application of special
functions.
