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Binary Effects on Supernovae

Published online by Cambridge University Press:  29 January 2014

Philipp Podsiadlowski
Philipp Podsiadlowski*
Affiliation:
Dept. of Astrophysics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford, OX1 3RH, United Kingdom email: podsi@astro.ox.ac.uk
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Abstract

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Here we review how binary interactions affect the final pre-supernova structure of massive stars and the resulting supernova explosions. (1) Binary-induced mass loss and mass accretion determine the final envelope structure, the mass, radius and chemical composition, which are mainly responsible for the supernova appearance and supernova (sub-)type. (2) Mass loss can also drastically change the core evolution and hence the final fate of a star; specifically, around 10 M⊙, it determines whether a star explodes in a supernova or forms a white dwarf, while for larger masses it can dramatically increase the minimum main-sequence mass above which a star is expected to collapse to a black hole. (3) Mass loss before the supernova directly affects the circumstellar medium (CSM) which can affect the supernova spectrum (e.g. account for the IIn phenomenon), produce powerful radio emission and, in extreme cases, lead to a strong interaction with the supernova ejecta and thus strongly modify the lightcurve shape; it may even be responsible for some of the superluminous supernovae that have recently been discovered.

Keywords

binaries (including multiple): closestars: mass losssupernovae: SN 1987Asupernova remnants
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S296: Supernova Environmental Impacts , January 2013 , pp. 45 - 52
Copyright
Copyright © International Astronomical Union 2014 

References

Brown, G. E., et al. 2001, NewA, 6, 457Google Scholar
Chevalier, R., 2012, ApJ, 752, 2Google Scholar
Fitzpatrick, B., 2012, D. Phil. Thesis (Oxford University)Google Scholar
Fryer, C. L., et al. 2007, PASP, 119, 1211Google Scholar
Gal-Yam, A., et al. 2007, ApJ 656, 372Google Scholar
Justham, S., Posiadlowski, Ph., & Vink, J.-S., 2013, submittedGoogle Scholar
Kotak, R. & Vink, J. S., 2006 A&A 460, L5Google Scholar
Maund, J. R., Smartt, S. J., Kudritzki, R. P., Podsiadlowski, Ph., & Gilmore, G. F., 2004, Nature, 427, 129CrossRefGoogle Scholar
Mohamed, S., Booth, R. & Podsiadlowski, Ph. 2013, in preparationGoogle Scholar
Morris, T. & Podsiadlowski, Ph. 2007, Science, 315, 1103CrossRefGoogle Scholar
Patat, F., et al., 2007, Science, 317, 924Google Scholar
Podsiadlowski, Ph., & Joss, P. C., 1989, Nature, 338, 401Google Scholar
Podsiadlowski, Ph., Joss, P. C., & Hsu, J. J. L., 1992, ApJ, 391, 246Google Scholar
Podsiadlowski, Ph., Joss, P. C., & Rappaport, S., 1990, A&A, 227, L9Google Scholar
Podsiadlowski, Ph. & Langer, N., et al. 2004, ApJ, 612, 1044CrossRefGoogle Scholar
Podsiadlowski, Ph., Morris, T. S., & Ivanova, N., 2007, in SN 1987A: 20 Years After, AIP Conf. Proc., Vol. 937, p. 125Google Scholar
Podsiadlowski, Ph., Rappaport, S., & Han, Z., 2003, MNRAS, 341, 385CrossRefGoogle Scholar
Quimby, R. M., et al. 2011, Nature, 474, 487CrossRefGoogle Scholar
Sana, H., et al. 2012, Science, 337, 444CrossRefGoogle Scholar
Smith, N., & McCray, R. 2007, ApJL, 671, L17CrossRefGoogle Scholar
Sugerman, B. E. K., et al. 2005, ApJS, 159, 60CrossRefGoogle Scholar
Wampler, E. J., et al. 1990, ApJL, 362, 13CrossRefGoogle Scholar
Weiler, K. W., et al. 1991, ApJ, 380, 161Google Scholar