Structure and Evolution of Stars Lecture 8
To the surface
T1 1 cm
T 1 < T2
T2 To the core
2
Log10 κ (m2 kg−1 )
1 0 −1 −2 −3
Log10 ρ (kg m−3 )
T + dT P + dP ρ + dρ
T + δT P + δP ρ + δρ
dr
T P ρ
T P ρ
!
dT dr
"
= rad
Unstable
T T !
dT dr
"
= rad
Stable
! !
r
""
dT dT dr dr
ad
ad
2
Log10 κ (m2 kg−1 )
1 0 −1 −2 −3
Log10 ρ (kg m−3 )
5 γ= 3
γ 5 = γ−1 2
Fg
FP,t
A dr
dm
r
FP,b
To the centre of the star
562
G. Meynet and A. Maeder: Stellar evolution with rotation. VIII.
Fig. 1. Stream lines of meridional circulation in a rotating 20 M! model with solar metallicity and vini = 300 km s−1 at the beginning of the H–burning phase (see text). The streamlines are in the meridian plane. In the upper hemisphere on the right section, matter is turning
