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Neutron Star Formation in Theoretical Supernovae — Low Mass Stars and White Dwarfs —

Published online by Cambridge University Press:  04 August 2017

Ken'ichi Nomoto
Ken'ichi Nomoto*
Affiliation:
Physics Department, Brookhaven National Laboratory on leave from the Department of Earth Science and Astronomy, University of Tokyo

Abstract

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The presupernova evolution of stars that form semi-degenerate or strongly degenerate O+Ne+Mg cores is discussed. For the 10–13 M⊙ stars, behavior of off-center neon flashes is crucial. The 8–10 M⊙ stars do not ignite neon and eventually collapse due to electron captures. Properties of supernova explosions and neutron stars expected from these low mass progenitors are compared with the Crab nebula. We also examine the conditions for which neutron stars form from accretion-induced collapse of white dwarfs in close binary systems.

Type
III. Neutron Star Formation in Theoretical Supernovae
Information
Symposium - International Astronomical Union , Volume 125: The Origin and Evolution of Neutron Stars , 1987 , pp. 281 - 303
Copyright
Copyright © Reidel 1987 

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