Hostname: page-component-8448b6f56d-wq2xx Total loading time: 0 Render date: 2024-04-19T14:01:54.208Z Has data issue: false hasContentIssue false
  • English
  • Français

A Single Degenerate Model for Ultra Super-Chandrasekhar Mass Progenitors of Type Ia Supernovae – Young and Low Metallicity Environments –

Published online by Cambridge University Press:  17 January 2013

Izumi Hachisu ,
Mariko Kato ,
Hideyuki Saio  and
Ken'ichi Nomoto
Izumi Hachisu
Affiliation:
University of Tokyo, Tokyo 153-8902, Japan email: hachisu@ea.c.u-tokyo.ac.jp
Mariko Kato
Affiliation:
Dept. of Astronomy, Keio University, Yokohama 223-8521, Japan
Hideyuki Saio
Affiliation:
Astronomical Institute, Tohoku University, Sendai 980-8578, Japan
Ken'ichi Nomoto
Affiliation:
Institute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa 277-8583, Japan
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Some Type Ia supernovae (SNe Ia) are suggested to have progenitor white dwarfs (WDs) with mass of up to 2.4–2.8 M⊙, highly exceeding the Chandrasekhar mass limit. We present a new single degenerate (SD) model for SNe Ia progenitors, in which the WD mass can increase by accretion up to 2.3 (2.7) M⊙ from the initial value of 1.1 (1.2) M⊙. The results are consistent with high luminosity SNe Ia such as SN 2003fg, SN 2006gz, SN 2007if, and SN 2009dc. There are three characteristic mass ranges of exploding WDs. In an extreme massive case, differentially rotating WDs explode as a SNe Ia soon after the WD mass exceeds 2.4 M⊙ because of a secular instability at T/|W|~0.14. For a mid mass range of MWD=1.5–2.4 M⊙, which is supported by differential rotation, it takes some spinning-down time until carbon is ignited to induce an SN Ia explosion. For a lower mass range of MWD=1.38–1.5 M⊙, they can be supported by rigid rotation until the angular momentum is lost. We also suggest the ultra super-Chandrasekhar mass SNe Ia are born in young and low metallicity environments.

Keywords

binaries: close — supernovae: individual (SN 2003fg, SN 2006gz, SN 2007if, SN 2009dc)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Issue S281: Binary Paths to Type Ia Supernovae Explosions , July 2011 , pp. 76 - 79
Copyright
Copyright © International Astronomical Union 2013

References

Chen, W.-C. & Li, X.-D. 2009, ApJ, 702, 686Google Scholar
Childress, N., et al. 2011, ApJ, 733:3Google Scholar
Hachisu, I. & Kato, M. 2001, ApJ, 558, 323CrossRefGoogle Scholar
Hachisu, I., Kato, M., & Nomoto, K. 1996, ApJ, 470, L97Google Scholar
Hachisu, I., Kato, M., & Nomoto, K. 1999a, ApJ, 522, 487Google Scholar
Hachisu, I., Kato, M., Saio, H., & Nomoto, K. 2012, ApJ, 744, 69Google Scholar
Hicken, M., et al. 2007, ApJ, 669, L17CrossRefGoogle Scholar
Howell, D., et al. 2006, Nature, 443, 308CrossRefGoogle Scholar
Ilkov, M. & Soker, N. 2012, MNRAS, 419, 1695CrossRefGoogle Scholar
Khan, R., Stanek, K. Z., Stoll, R., & Prieto, J. L. 2011, ApJ, 737, L24Google Scholar
Liu, W.-M., Chen, W.-C., Wang, B., & Han, Z. W. 2010, A&A, 523, A3Google Scholar
Nomoto, K., Saio, H., Kato, M., & Hachisu, I. 2007, ApJ, 663, 1269CrossRefGoogle Scholar
Scalzo, R. A., et al. 2010, ApJ, 713, 1073Google Scholar
Silverman, J. M., et al. 2011, MNRAS, 410, 585Google Scholar
Taubenberger, S., et al. 2011, MNRAS, 412, 2735Google Scholar
Yamanaka, M., et al. 2009, ApJ, 707, L118Google Scholar
Yoon, S.-C. & Langer, N. 2004, A&A, 419, 623Google Scholar
Yoon, S.-C. & Langer, N. 2005, A&A, 435, 967Google Scholar