2007
DOI: 10.1086/511781
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Making a Short Gamma-Ray Burst from a Long One: Implications for the Nature of GRB 060614

Abstract: The absence of a supernova accompanying the nearby long GRB 060614 poses a great puzzle about the progenitor of this event and challenges the current GRB classification scheme. This burst displays a short-hard emission episode followed by extended soft emission with strong spectral evolution. Noticing that this burst has an isotropic gamma-ray energy only ∼8 times that of GRB 050724, a good candidate of merger-type short GRBs, we generate a "pseudo" burst that is ∼8 times less energetic than GRB 060614 based o… Show more

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Cited by 234 publications
(285 citation statements)
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“…This is also consistent with the empirical relation between E p and Γ (measured by BAT) for a number of bursts (Zhang et al 2007a). Assuming this value for E p , we derive the following values: E p,i = 383 +346 −95 keV (rest-frame peak energy) and E iso = (6.2 ± 0.7) × 10 52 erg (isotropic-equivalent released energy in the rest-frame 1−10 4 keV energy band, errors at 90%).…”
Section: Swift-batsupporting
confidence: 90%
“…This is also consistent with the empirical relation between E p and Γ (measured by BAT) for a number of bursts (Zhang et al 2007a). Assuming this value for E p , we derive the following values: E p,i = 383 +346 −95 keV (rest-frame peak energy) and E iso = (6.2 ± 0.7) × 10 52 erg (isotropic-equivalent released energy in the rest-frame 1−10 4 keV energy band, errors at 90%).…”
Section: Swift-batsupporting
confidence: 90%
“…3.11). The origin of the other two bursts (GRB 060505 and GRB 060614) remains controversial: they have been argued to be linked to the explosions of massive stars that produce very little radioactive nickel and thus no radioactivity-driven SN emission (Fynbo et al 2006;Della Valle et al 2006a;Gal-Yam et al 2006;Thöne et al 2008;McBreen et al 2008;Tominaga et al 2007;Fryer et al 2006Fryer et al , 2007, whereas other indicators point to an origin in merging compact objects despite their longer duration, which would naturally not be accompanied by SN emission (Gehrels et al 2006;Zhang et al 2007;Ofek et al 2007;Kann et al 2008;Krimm et al 2009). …”
Section: Fig 12mentioning
confidence: 99%
“…In the literature possible explanation for this have been that not enough 56 Ni is formed in the explosion (Tominaga et al 2007), or that this is a very long and energetic ''short'' burst (Zhang et al 2007). Here we give a possible interpretation of this phenomena within our model.…”
Section: Sn-less Grbs In Our Modelmentioning
confidence: 99%