The association of GRB 060218 with a supernova and the evolution of the shock wave

Campana, S.; Mangano, V.; Blustin, A. J.; Brown, P. J.; Burrows, D. N.; Chincarini, G.; Cummings, J. R.; Cusumano, G.; Valle, M. Della; Malesani, D.; Mészáros, P.; Nousek, J. A.; Page, M. J.; Sakamoto, T.; Waxman, Eli; Zhang, Bing; Dai, Z. G.; Gehrels, N.; Immler, S.; Marshall, F. E.; Mason, K. O.; Moretti, A.; O’Brien, P. T.; Osborne, J. P.; Page, K. L.; Romano, P.; Roming, P. W. A.; Tagliaferri, G.; Cominsky, L.; Giommi, P.; Godet, O.; Kennea, J. A.; Krimm, H. A.; Angelini, L.; Barthelmy, S. D.; Boyd, Patricia T.; Palmer, D. M.; Wells, A.; White, N. E.

doi:10.1038/nature04892

Cited by 744 publications

(1,051 citation statements)

References 24 publications

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“…gamma-ray bursts with peak energies below approximately 50 keV. Observational evidence suggests that the radio and high-energy emission is due to the breakout of a relativistic shock from the surrounding massive wind of the progenitor star [2,[15][16][17][18]. Apart from SN 2003dh (and possibly SN 2012bz), the best-studied supernovae related to gamma-ray bursts are all members of this class.…”

Section: Supernovae Associated With Long-duration Gamma-ray Burstsmentioning

confidence: 99%

The supernova–gamma-ray burst–jet connection

Hjorth

2013

Phil. Trans. R. Soc. A.

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The observed association between supernovae and gamma-ray bursts represents a cornerstone in our understanding of the nature of gamma-ray bursts. The collapsar model provides a theoretical framework for this connection. A key element is the launch of a bipolar jet (seen as a gamma-ray burst). The resulting hot cocoon disrupts the star, whereas the 56 Ni produced gives rise to radioactive heating of the ejecta, seen as a supernova. In this discussion paper, I summarize the observational status of the supernova–gamma-ray burst connection in the context of the ‘engine’ picture of jet-driven supernovae and highlight SN 2012bz/GRB 120422A—with its luminous supernova but intermediate high-energy luminosity—as a possible transition object between low-luminosity and jet gamma-ray bursts. The jet channel for supernova explosions may provide new insights into supernova explosions in general.

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Section: Supernovae Associated With Long-duration Gamma-ray Burstsmentioning

confidence: 99%

The supernova–gamma-ray burst–jet connection

Hjorth

2013

Phil. Trans. R. Soc. A.

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“…The existence of an additional blackbody component in the prompt X-ray spectrum of GRB 060218 (Campana et al 2006) and GRB 100316D (Starling et al 2011) has been reported. The blackbody temperature is stable in the range of 0.1-0.2 keV up to several hundreds of seconds after the trigger, and then, decreases to < 0.01 keV.…”

Section: Additional Blackbody Component In X-ray Spectrummentioning

confidence: 94%

“…While GRB 060218 and GRB 100316D show a duration of several thousands of seconds (Campana et al 2006;Starling et al 2011), SN-GRBs with a duration of a several tens to hundreds of seconds are also common. Although the durations of GRB 060218 and GRB 100316D are exceptionally long, the rest of the sample is well within the duration distribution of typical long GRBs (Figure 2).…”

Section: Durationsmentioning

confidence: 99%

GRB Prompt X-ray Emission

Sakamoto

2011

Proc. IAU

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Abstract. I present the observational properties of the prompt emission of supernova associated GRBs (SN-GRBs) focusing on temporal and spectral characteristics. I compare the properties of SN-GRBs with typical long GRBs to see whether there is a distinct difference or not. Furthermore, I present our attempt to search for hard X-ray emission prior to the discovery date from optically identified type Ibc supernovae using Swift BAT survey data.

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“…One then might get a long X-ray flash visible at large angles. An example might be XRF 060218 (Campana et al 2006). …”

Section: Discussionmentioning

confidence: 99%

Models for GRBs and diverse transients

Woosley

Zhang

2007

Phil. Trans. R. Soc. A.

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The observational diversity of gamma-ray bursts (GRBs) has been increasing, and the natural inclination is a proliferation of models. We explore the possibility that at least part of this diversity is a consequence of a single basic model for the central engine operating in a massive star of variable mass, differential rotation rate and mass loss rate. Whatever that central engine may be-and here the collapsar is used as a reference point-it must be capable of generating both a narrowly collimated, highly relativistic jet to make the GRB and a wide angle, sub-relativistic outflow responsible for exploding the star and making the supernova bright. To some extent, the two components may vary independently; therefore, it is possible to produce a variety of jet energies and supernova luminosities. We explore, in particular, the production of low-energy bursts and find a lower limit of approximately 10 48 erg s K1 to the power required for a jet to escape a massive star before that star either explodes or is accreted. Lower energy bursts and 'suffocated' bursts may be particularly prevalent when the metallicity is high, i.e. in the modern universe at low red shift.

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The association of GRB 060218 with a supernova and the evolution of the shock wave

Cited by 744 publications

References 24 publications

The supernova–gamma-ray burst–jet connection

The supernova–gamma-ray burst–jet connection

GRB Prompt X-ray Emission

Models for GRBs and diverse transients

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