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Final evolution of super-AGB stars and supernovae triggered by electron capture
Leung, Shing-Chi; Nomoto, Ken'ichi
AA(Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo, Kashiwa 277-8583, Japan 0000-0002-4972-3803), AB(Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo, Kashiwa 277-8583, Japan 0000-0001-9553-0685)
Publications of the Astronomical Society of Australia, Volume 36, id. e006 (PASA Homepage)
Publication Date:
Astronomy Keywords:
AGB stars, electron-capture supernovae, hydrodynamics, nucleosynthesis
Abstract Copyright:
2019: Astronomical Society of Australia
Bibliographic Code:


Stars of 8-10 M&sun; form a strongly electron-degenerate oxygen-neon-magnesium core which is more massive than ˜1.1 M&sun;, and become super-Asymptotic Giant Branch stars. The oxygen-neon-magnesium core increases its mass through H and He shell burning. The core contracts accordingly and the central density increases. In the high density core, electron capture takes place and further boosts the core contraction. When electron capture on 20Ne starts, it induces oxygen-neon deflagration. It remains a theoretical question whether neutron star can be formed after the deflagration has started. If the star collapses, the following explosion is known as an electron capture supernova. In this article, we give a brief overview on the development of idea in the presupernova evolution and the hydrodynamics behaviour of electron capture supernovae. Using standard stellar evolutionary models that show rather high ignition density, we show that the collapse can occur in a wide range of model parameter. However, future study remains important. We also review the possible observables of electron capture supernovae and discuss their applications to the light curve model for the Crab supernova 1054.
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