Stellar evolution (II)
28 Abril 2020, 13:00 • Israel Matute
Evolution of low-mass stars (~1 M☉)
Formation of a degenerate Helium nucleus (ashes) and the Helium flash
Stable burning of Helium into Carbon and Oxygen
Helium and hydrogen burning in shells
(Small) Helium flashes in shells
White dwarf and Planetary Nebulae phase
Evolution of intermediate-mass stars (~5 M☉) (part I)
No degenerate Helium nuclei and therefore no Helium flash
Stable burning of Helium into Carbon and Oxygen