Properties of some well-known Main Sequence Stars..
Aller1961 & Clayton Main Seq. chemistry X=0.5976, Y=0.3825, Z=0.199
STAR       Derived Properties [Book] || Observed Properties || III=Giant
NAME(Constella) M/Msun R/Rsun  L/Lsun Distance mag m Spectrum->Tsurf
Eltanin(Draco)                 145    100 LY   2.22   K5 III   3780K
Enif(Pegasus)                  5800   780 LY   2.31   K2 Ib    4460K
Fomalhaut(P.A)           2(bhm)14     23 LY    1.17   A3 V     8990K
Gienah(Corvus)                 1200   450 LY   2.6    B8 III   13400K
Agena(Centaur)                 10,000 490 LY   0.66   B1 II    24200K
HELP NOTES: The internal structure of the stars is still under test.
Based on theoretical analysis, we may consider stars as Standard
Model polytropes with n=3 and gamma = 4/3.  These models include the
gas & radiation pressure. Lighter stars with no radiation pressure are
represented by polytropes of with n=1.5 and gamma=5/3.  As stars age
they become more inhomogeneous, finally growing H-depleted cores in 
central regions that may collapse to a white dwarf state with ejection
of a planetary nebula. Stars have lifetimes like 13x10**9(Msun/M)**2
years, so that heavier stars are more likely to be mature, with denser
core regions. STARCAL considers the equation of radiative equilibrium
to apply to the determination of L_radiation(r), the radiative part
energy transmission partition, so that dT/dr is not determined by L(r),
but by the hydrostatic equilibrium with gas plus radiation pressure
as described by the n=3, gamma=4/3 polytropes. This gets good results.
$