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Spin-Up/Spin-Down Models

Published online by Cambridge University Press:  17 January 2013

R. Di Stefano ,
R. Voss  and
J. Claeys
R. Di Stefano
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA email: rd@cfa.harvard.edu
R. Voss
Affiliation:
Department of Astrophysics/IMAPP, Radboud University Nijmegen, PO Box 9010, NL-6500 GL Nijmegen, the Netherlands email: R.Voss@astro.ru.nl, J.Claeys@astro.ru.nl
J. Claeys
Affiliation:
Department of Astrophysics/IMAPP, Radboud University Nijmegen, PO Box 9010, NL-6500 GL Nijmegen, the Netherlands email: R.Voss@astro.ru.nl, J.Claeys@astro.ru.nl
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Abstract

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Angular momentum transport plays an important role in mass transfer systems, and can significantly spin up an accreting star. When the accretor is a white dwarf (WD) on its way to becoming a Type Ia supernova (SN Ia), the spin up of the WD can have significant consequences for the appearance of the progenitor, the characteristics of the explosion and its aftermath, the geometry of the supernova remnant, and for single-degenerate models, the appearance of the donor star post-explosion. These consequences can be “game changers”, altering results that have long been taken for granted. We discuss key features of our spin-up/spin-down models and their implications. We relate our models to work still needed to address the difficult physical issues related to angular momentum transport and its effects on the properties and appearance of Type Ia supernova progenitors.

Keywords

stars: white dwarfssupernovae — accretionaccretion disks
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Issue S281: Binary Paths to Type Ia Supernovae Explosions , July 2011 , pp. 64 - 67
Copyright
Copyright © International Astronomical Union 2013

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