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A hypernova model for the supernova associated with the γ-ray burst of 25 April 1998

Author

Listed:
  • K. Iwamoto

    (School of Science, University of Tokyo)

  • P. A. Mazzali

    (Osservatorio Astronomico di Trieste)

  • K. Nomoto

    (School of Science, University of Tokyo
    Research Centre for the Early Universe, School of Science, University of Tokyo)

  • H. Umeda

    (School of Science, University of Tokyo
    Research Centre for the Early Universe, School of Science, University of Tokyo)

  • T. Nakamura

    (School of Science, University of Tokyo)

  • F. Patat

    (European Southern Observatory)

  • I. J. Danziger

    (Osservatorio Astronomico di Trieste)

  • T. R. Young

    (School of Science, University of Tokyo)

  • T. Suzuki

    (School of Science, University of Tokyo
    Research Centre for the Early Universe, School of Science, University of Tokyo)

  • T. Shigeyama

    (School of Science, University of Tokyo
    Research Centre for the Early Universe, School of Science, University of Tokyo)

  • T. Augusteijn

    (European Southern Observatory)

  • V. Doublier

    (European Southern Observatory)

  • J.-F. Gonzalez

    (European Southern Observatory)

  • H. Boehnhardt

    (European Southern Observatory)

  • J. Brewer

    (European Southern Observatory)

  • O. R. Hainaut

    (European Southern Observatory)

  • C. Lidman

    (European Southern Observatory)

  • B. Leibundgut

    (European Southern Observatory)

  • E. Cappellaro

    (Osservatorio Astronomico di Padova)

  • M. Turatto

    (Osservatorio Astronomico di Padova)

  • T. J. Galama

    (Astronomical Institute Anton Pannekoek, University of Amsterdam, and Center for High Energy Astrophysics)

  • P. M. Vreeswijk

    (Astronomical Institute Anton Pannekoek, University of Amsterdam, and Center for High Energy Astrophysics)

  • C. Kouveliotou

    (NASA Marshall Space Flight Center, ES-84)

  • J. van Paradijs

    (Astronomical Institute Anton Pannekoek, University of Amsterdam, and Center for High Energy Astrophysics
    University of Alabama)

  • E. Pian

    (Istituto Tecnologie e Studio Radiazioni Extraterrestri, CNR)

  • E. Palazzi

    (Istituto Tecnologie e Studio Radiazioni Extraterrestri, CNR)

  • F. Frontera

    (Istituto Tecnologie e Studio Radiazioni Extraterrestri, CNR)

Abstract

The discovery of the unusual supernova SN1998bw, and its possible association with the γ-ray burst GRB 9804251,2,3, provide new insights into the explosion mechanism of very massive stars and the origin of some classes of γ-ray bursts. Optical spectra indicate that SN1998bw is a type Ic supernova3,4, but its peak luminosity is unusually high compared with typical type Ic supernovae3. Here we report our findings that the optical spectra and the light curve of SN1998bw can be well reproduced by an extremely energetic explosion of a massive star composed mainly of carbon and oxygen (having lost its hydrogen and helium envelopes). The kinetic energy of the ejecta is as large as +(2–5)× 1052 erg, more than ten times that of previously observed supernovae. This type of supernova could therefore be termed ‘hypernova’. The extremely large energy suggests the existence of a new mechanism of massive star explosion that can also produce the relativistic shocks necessary to generate the observed γ-rays.

Suggested Citation

  • K. Iwamoto & P. A. Mazzali & K. Nomoto & H. Umeda & T. Nakamura & F. Patat & I. J. Danziger & T. R. Young & T. Suzuki & T. Shigeyama & T. Augusteijn & V. Doublier & J.-F. Gonzalez & H. Boehnhardt & J., 1998. "A hypernova model for the supernova associated with the γ-ray burst of 25 April 1998," Nature, Nature, vol. 395(6703), pages 672-674, October.
    • Handle: RePEc:nat:nature:v:395:y:1998:i:6703:d:10.1038_27155
    DOI: 10.1038/27155
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