'Shell burning' presentation slideshows

Chapter 17 Star Stuff

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Post-Main Sequence Evolution of Massive Stars

Post-Main Sequence Evolution of Massive Stars. Stars of more than 8 solar masses leave behind neutron stars and black holes and typically explode as supernovae. But first, NOVAE from WDs. Back to binary star evolution: More massive star leaves MS first, becomes RG, then WD

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HR Diagram for nearby stars atlasoftheuniverse/hr.html

HR Diagram for nearby stars http://www.atlasoftheuniverse.com/hr.html. Temperature. Main Sequence H burning pp/CNO exhaust core H Contraction Density/T inc. H shell burning Expansion Core He burning He shell burning. What happens at hydrogen exhaustion.

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Chapter 14: Star Stuff

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Late Burning Stages

Late Burning Stages. Late Burning Stages. Late Burning Stages. Late Burning Stages. Late Burning Stages. Q He ~Q C+C ~Q O+O but ? He >> ? C+C >> ? O+O. O burning; ?? ? > 10 20 erg g -1 s -1. C burning; ?? ? > 10 17 erg g -1 s -1. He burning; ?? ? ~ 10 12 erg g -1 s -1.

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The origin of heavy elements in the solar system

The origin of heavy elements in the solar system. (Pagel, Fig 6.8). each process contribution is a mix of many events !. The sites of the s-process. weak s-process: core He/ shell C burning in massive stars. main s-process: He shell flashes in low mass TP-AGB stars. approx. steady flow.

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