  This paper reviews the physics of stars, the type, structure, evolution and
stability. Simple thermodynamics and statistical mechanics are used to show the
inner working of white dwarf and neutron stars. The major concentration of the
paper will be on white dwarf stars although in some places references will also
be made to neutron stars where the relations can be extended easily. It can be
shown that a maximum mass limit is attached to each type of star which can be
derived rigorously. Maximum entropy can be used to show that the gravitational
contraction is balanced by the degeneracy pressure created by the electrons in
the case of white dwarfs, and neutrons and protons which constitute the matter
of the neutron star. Finally the kinetic equations which describe the
luminosity of the star and the radiative transfer are introduced.
