2/12/2024 0 Comments Third dredge up final core mass![]() ![]() Weinberg (World Scientific), 95īarkat, Z., Rakavy, G., & Sack, N. ![]() 1996, Supernovae and Nucleosynthesis: an Investigation of the History of Matter from the Big Bang to the Present (Princeton Un. Another section addresses the equally complex topic of binary-star evolution, which is essential to understanding the origin of Type Ia supernovae and probably of most stripped-envelope supernovae (Types IIb, Ib, and Ic).Ībel, T., Anninos, P., Norman, M. A section of the chapter is devoted to the complex effects of rotation on single-star evolution. More massive stars may undergo thermonuclear explosions owing to pair instabilities in their oxygen cores. In this range, some stars explode by ejecting their envelopes while others may become black holes. Stars of ZAMS mass between 13 and about 70 solar masses undergo collapse of their iron cores. At present, it is difficult to know which of these stars undergo collapse, and perhaps explode and whether they have carbon-oxygen or oxygen-neon-magnesium cores. The evolution of stars of ZAMS mass 6–13 solar masses is exceedingly complex, involving degenerate cores, episodes of dredge-up of matter from their interiors, thermal pulses, off center ignition of neon and oxygen, mass loss, and more. Single stars of zero-age main-sequence (ZAMS) mass up to at least 6 solar masses become white dwarfs that will not explode as supernovae. In this chapter describes presupernova evolution. ![]()
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