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.
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