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9 - The GRB–supernova connection

Published online by Cambridge University Press:  05 December 2012

By
Jens Hjorth  and
Joshua S. Bloom
Edited by
Chryssa Kouveliotou ,
Ralph A. M. J. Wijers  and
Stan Woosley
Jens Hjorth
Affiliation:
Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen Ø, Denmark
Joshua S. Bloom
Affiliation:
Astronomy Department, University of California, 601 Campbell Hall, Berkeley, CA 94720, USA
Chryssa Kouveliotou
Affiliation:
NASA-Marshall Space Flight Center, Huntsville
Ralph A. M. J. Wijers
Affiliation:
Universiteit van Amsterdam
Stan Woosley
Affiliation:
University of California, Santa Cruz
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Summary

Introduction

The discovery and localization of the first afterglows of GRBs rapidly led to the establishment of the long-sought distance scale for the sources (see Chapter 4), which began an earnest observational hunt for their progenitors. A preponderance of evidence linked long-duration, soft-spectrum GRBs with the death of massive stars. The observations of the GRB-supernova (SN) connection, the main subject of this chapter, present the most direct evidence of this physical link.

Well before the afterglow era, Paczyński (1986) noted that “cosmological” distances of GRBs would imply that the energy release in gamma rays would be comparable to the energy release in a typical SN explosion. Seen as more than just a coincidence, this energetics connection between GRBs and the death of massive stars was fleshed out into what is now referred to as the collapsar model (Woosley 1993, 1996, MacFadyen & Woosley 1999). Briefly, the collapsar involves the core-collapse explosion of a stripped-envelope massive star. Matter flows towards a newly formed black hole or rapidly spinning, highly magnetized neutron star (“magnetar”; e.g., Bucciantini et al. 2009). Powerful jets plow through the collapsing star along the spin axis, eventually obtain relativistic speeds, and produce GRBs. Enough 56Ni is produced near the central compact source to power a supernova explosion of the star. The original “failed Ib” model posited that little 56Ni would be produced during core collapse of a massive star that produces a GRB, and thus no traditional SN would be visible.

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Gamma-ray Bursts , pp. 169 - 190
Publisher: Cambridge University Press
Print publication year: 2012

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  • The GRB–supernova connection
    • By Jens Hjorth, Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen Ø, Denmark, Joshua S. Bloom, Astronomy Department, University of California, 601 Campbell Hall, Berkeley, CA 94720, USA
  • Edited by Chryssa Kouveliotou, NASA-Marshall Space Flight Center, Huntsville, Ralph A. M. J. Wijers, Universiteit van Amsterdam, Stan Woosley, University of California, Santa Cruz
  • Book: Gamma-ray Bursts
  • Online publication: 05 December 2012
  • Chapter DOI: https://doi.org/10.1017/CBO9780511980336.010
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  • The GRB–supernova connection
    • By Jens Hjorth, Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen Ø, Denmark, Joshua S. Bloom, Astronomy Department, University of California, 601 Campbell Hall, Berkeley, CA 94720, USA
  • Edited by Chryssa Kouveliotou, NASA-Marshall Space Flight Center, Huntsville, Ralph A. M. J. Wijers, Universiteit van Amsterdam, Stan Woosley, University of California, Santa Cruz
  • Book: Gamma-ray Bursts
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  • Chapter DOI: https://doi.org/10.1017/CBO9780511980336.010
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  • The GRB–supernova connection
    • By Jens Hjorth, Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen Ø, Denmark, Joshua S. Bloom, Astronomy Department, University of California, 601 Campbell Hall, Berkeley, CA 94720, USA
  • Edited by Chryssa Kouveliotou, NASA-Marshall Space Flight Center, Huntsville, Ralph A. M. J. Wijers, Universiteit van Amsterdam, Stan Woosley, University of California, Santa Cruz
  • Book: Gamma-ray Bursts
  • Online publication: 05 December 2012
  • Chapter DOI: https://doi.org/10.1017/CBO9780511980336.010
Available formats
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