Stellar Evolution (III)

30 Abril 2020, 14:00 • Israel Matute

Evolution of intermediate-mass stars (~5 M☉)

• Helium and hydrogen burning in shells

• (small) Helium flashes in shells

• White dwarf and Planetary Nebulae phase

Evolution of the most massive stars

• Similar evolution to intermediate stars but at a much higher temporal pace.

• Most massive stars end up with an iron core and continuous layers burning the less heavy elements: Silicon, Oxygen, Neon, carbon, He, and H.

• Depending on whether the final core mass reaches the Chandrasekhar limit different end scenarios are described: neutron star, Type-II supernova or black-holes.

• These stars lose a large fraction of their mass before the end-stage. Large enrichment of ISM. Examples described in class.