2015
DOI: 10.1088/0004-637x/808/2/190
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GRB 140619b: A Short GRB From a Binary Neutron Star Merger Leading to Black Hole Formation

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Cited by 28 publications
(99 citation statements)
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“…This result is also in good agreement with the NS-NS binaries observed within our Galaxy: only a subset of them has a total mass larger than the NS critical mass M NS crit and can form a BH in their merging process [10] if we assume that M NS crit = 2.67M � for a non-rotating, globally neutral NS within the NL3 nuclear model [87]. In this light S-GRBs are very important for inferring constraints on M NS crit , on the NS equation of state, and on the minimum mass of the newly-formed BH.…”
Section: The S-grbs In the Ns-ns Merger Paradigmsupporting
confidence: 90%
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“…This result is also in good agreement with the NS-NS binaries observed within our Galaxy: only a subset of them has a total mass larger than the NS critical mass M NS crit and can form a BH in their merging process [10] if we assume that M NS crit = 2.67M � for a non-rotating, globally neutral NS within the NL3 nuclear model [87]. In this light S-GRBs are very important for inferring constraints on M NS crit , on the NS equation of state, and on the minimum mass of the newly-formed BH.…”
Section: The S-grbs In the Ns-ns Merger Paradigmsupporting
confidence: 90%
“…The spectrum of the P-GRB is determined by the geometry of the pair-creation region: in the case of the spherically symmetric dyadosphere, the P-GRB spectrum is generally described by a single thermal component [42]. [10,63]; in the case of an axially symmetric dyadotorus, the resulting P-GRB spectrum is a convolution of thermal spectra of different temperatures which resembles more a power-law spectral energy distribution with an exponential cutoff [64,65].…”
Section: The Fireshell Modelmentioning
confidence: 99%
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