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Evolution of Rotating White Dwarfs in Close Binaries and Diversity of Type Ia Supernovae

Published online by Cambridge University Press:  26 May 2016

Tatsuhiro Uenishi ,
Ken'ichi Nomoto  and
Izumi Hachisu
Tatsuhiro Uenishi
Affiliation:
Department of Astronomy, School of Science, University of Tokyo, Hongo 7-3-1, Bunkyo-ku, Tokyo 113-0033, Japan
Ken'ichi Nomoto
Affiliation:
Department of Astronomy, School of Science, University of Tokyo, Hongo 7-3-1, Bunkyo-ku, Tokyo 113-0033, Japan
Izumi Hachisu
Affiliation:
Department of Earth Science and Astoronomy, College of Arts and Science, University of Tokyo Komaba 3-8-1, Meguro-ku, Tokyo 153-8902, Japan

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Type Ia supernovae are very good, but not perfect, standard candles, because their observed brightness shows a little diversity. The origin of this dibersity needs to be understood for the application to cosmology.

In close binary systems, a white dwarf must be rotating faster and faster as it gains angular momentum from the accretion disk. Its rapid rotation affects its final mass and strucure just before a supernova expolosion. Brightness of supernovae can be changed if mass of their progenitors have some diversity.

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Information
Symposium - International Astronomical Union , Volume 208: Astrophysical Supercomputing using Particle Simulations , 2003 , pp. 459 - 460
Copyright
Copyright © Astronomical Society of the Pacific 2003