imf - cosmos.phy.tufts.educosmos.phy.tufts.edu/~danilo/ast121/material/lecturefigures_20_25.pdf ·...
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IMF
D burning
Envelope becomes radiative
Core becomes convective
M~0.8 MsunM~1 Msun
M~2 Msun
M/Msun<0.8
0.8<M/Msun<2
M/Msun>2
5 Msun star with He core and H-burning shell shortly after shell ignition
5 Msun star on the early asymptotic giant branch with C-O core and H- and He-burning shells. The scale of the shells and core has been increased by x100.
M3, old globular cluster
MS
TO
BS
P-AGB
HB
AGB
RGB
SGB
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