Structure and Evolution of Stars Lecture 9
R C Smith 1983 L ∝ L!
!
M M!
"2.3
L ∝ L!
!
M M!
"4
1993A&AS...98..477M
The Mass Continuity Equation dr
dmi r
M
dm = 4πr2 ρ dr
The Hydrostatic Equilibrium Equation Fg
FP,t
A dr
dm
r
FP,b
To the centre of the star
dP Mr ρ = −G 2 dr r
P(m) inner models P(m) outer models
∗∗∗ ∗
P(m)
∗
∗
∗
∗
m
∗
Model Fit
∗ M∗
1 Msun m(r)/M 4 density 2
0
15
convection
`Real’ Stellar Model:
pressure 10
M = 1 M!
5 luminosity 7
6
temperature
5 opacity 4 2
4
6
3 Msun
4 2 density 0 m(r)/M
-2 -4
15
pressure
`Real’ Stellar Model:
convection 10
M = 3 M!
5 luminosity 7 temperature 6
5 opacity 4 0.5
1
15 Msun
4 2 density 0 m(r)/M
-2 -4
15
pressure
`Real’ Stellar Model:
convection 10
M = 15 M!
5 luminosity 7 temperature 6
5 opacity 4 1
2
3
