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