Long gamma ray bursts from binary black holes

Janiuk, Agnieszka; Charzyński, Szymon; Bejger, M.

doi:10.1051/0004-6361/201322165

Cited by 15 publications

(11 citation statements)

References 63 publications

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“…In principle, mergers of binary BHs may be associated with an electromagnetic emission (a GRB), if a sufficient supply of matter for the accretion is involved at any stage of the merger, or after the GW event. As hypothesized in our previous work [4], a merger of a massive, rotating star with a companion BH, in a system that evolved from a high mass X-ray binary, may result in the collapse of the star's core. The merger of the collapsed core, which is a newly formed BH, with its companion, would be then the source of a transient emission seen in GWs.…”

Section: Introductionmentioning

confidence: 61%

On the possible gamma-ray burst–gravitational wave association in GW150914

et al. 2017

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Data from the Fermi Gamma-ray Burst Monitor satellite observatory suggested that the recently discovered gravitational wave source, a pair of two coalescing black holes, was related to a gamma-ray burst. The observed high-energy electromagnetic radiation (above 50 keV) originated from a weak transient source and lasted for about 1 second. Its localization is consistent with the direction to GW150914. We speculate about the possible scenario for the formation of a gamma-ray burst accompanied by the gravitational-wave signal. Our model invokes a tight binary system consisting of a massive star and a black hole which leads to the triggering of a collapse of the star's nucleus, the formation of a second black hole, and finally to the binary black hole merger. For the most-likely configuration of the binary spin vectors with respect to the orbital angular momentum in the GW150914 event, the recoil speed (kick velocity) acquired by the final black hole through gravitational wave emission is of the order of a few hundred km/s and this might be sufficient to get it closer to the envelope of surrounding material and capture a small fraction of matter from the remnant of the host star. The gamma-ray burst is produced by the accretion of this remnant matter onto the final black hole. The moderate spin of the final black hole suggests that the gamma-ray burst jet is powered by weak neutrino emission rather than the Blandford-Znajek mechanism, and hence explains the low power available for the observed GRB signal.

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Section: Introductionmentioning

confidence: 61%

On the possible gamma-ray burst–gravitational wave association in GW150914

et al. 2017

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“…The two BH masses are determined by the signal, and this may be an independent method to measure the mass of GRB central BHs (see, e.g. an earlier investigation by Janiuk et al 2013a).…”

Section: Conclusion and Discussionmentioning

confidence: 99%

A Method to Constrain Mass and Spin of GRB Black Holes Within the Ndaf Model

Liu

Xue

Zhao

et al. 2016

ApJ

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Black holes (BHs) hide themselves behind various astronomical phenomena, and their properties, i.e., mass and spin, are usually difficult to constrain. One leading candidate for the central engine model of gamma-ray bursts (GRBs) invokes a stellar mass BH and a neutrino-dominated accretion flow (NDAF), with the relativistic jet launched due to neutrino-anti-neutrino annihilations. Such a model gives rise to a matter-dominated fireball, and is suitable to interpret GRBs with a dominant thermal component with a photospheric origin. We propose a method to constrain BH mass and spin within the framework of this model, and apply the method to a thermally-dominant GRB 101219B whose initial jet launching radius r 0 is constrained from the data. Using our numerical model of NDAF jets, we estimate the following constraints on the central BH: mass M BH ∼ 5 − 9 M ⊙ , spin parameter a * 0.6, and disk mass 3 M ⊙ M disk 4 M ⊙ . Our results also suggest that the NDAF model is a competitive candidate for the central engine of GRBs with a strong thermal component.

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“…Our model invokes coalescence of a collapsing star's nucleus that forms a BH, with its companion BH in a binary system [12,30]. We find that the recoil velocity acquired by the final BH through the GW emission allows it to take only a small fraction of matter from the host star, provided specific configuration of the binary spin vectors with the orbital angular momentum.…”

Section: Gravitational Wave Source Gw150914mentioning

confidence: 95%

Black Hole Accretion in Gamma Ray Bursts

et al. 2017

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Abstract:We study the structure and evolution of the hyperaccreting disks and outflows in the gamma ray bursts central engines. The torus around a stellar mass black hole is composed of free nucleons, Helium, electron-positron pairs, and is cooled by neutrino emission. Accretion of matter powers the relativistic jets, responsible for the gamma ray prompt emission. The significant number density of neutrons in the disk and outflowing material will cause subsequent formation of heavier nuclei. We study the process of nucleosynthesis and its possible observational consequences. We also apply our scenario to the recent observation of the gravitational wave signal, detected on 14 September 2015 by the two Advanced LIGO detectors, and related to an inspiral and merger of a binary black hole system. A gamma ray burst that could possibly be related with the GW150914 event was observed by the Fermi satellite. It had a duration of about 1 s and appeared about 0.4 s after the gravitational-wave signal. We propose that a collapsing massive star and a black hole in a close binary could lead to the event. The gamma ray burst was powered by a weak neutrino flux produced in the star remnant's matter. Low spin and kick velocity of the merged black hole are reproduced in our simulations. Coincident gravitational-wave emission originates from the merger of the collapsed core and the companion black hole.

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Long gamma ray bursts from binary black holes

Cited by 15 publications

References 63 publications

On the possible gamma-ray burst–gravitational wave association in GW150914

On the possible gamma-ray burst–gravitational wave association in GW150914

A Method to Constrain Mass and Spin of GRB Black Holes Within the Ndaf Model

Black Hole Accretion in Gamma Ray Bursts

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