Accretion Models of Gamma-Ray Bursts

By Ramesh Narayan, T. Piran, Pawan Kumar. 2001

346 citations recorded by the source corpus.

Many models of gamma-ray bursts (GRBs) involve accretion onto a compact object, usually a black hole, at a mass accretion rate on the order of a fraction of a solar mass per second. If the accretion disk is larger than a few tens or hundreds of Schwarzschild radii, the accretion will proceed via a convection-dominated accretion flow (CDAF) in which most of the matter escapes to infinity rather than falling onto the black hole. Models involving the mergers of black hole-white dwarf binaries and black hole-helium star binaries fall in this category. These models are unlikely to produce GRBs since very little mass reaches the black hole. If the accretion disk is smaller, then accretion will proceed via neutrino cooling in a neutrino-dominated accretion disk (NDAF) and most of the mass will reach the center. Models involving the mergers of double neutron star binaries and black hole-neutron star binaries fall in this category and are capable of producing bright GRBs. If the viscosity parameter α in the NDAF has a standard value of ~0.1, these mergers can explain short GRBs with durations under a second, but they are unlikely to produce long GRBs with durations of tens or hundred of seconds. If the accretion disk is fed by fallback of material after a supernova explosion, as in the collapsar model, then the timescale of the burst is determined by fallback, not accretion. Such a model can produce long GRBs. Fallback models again require that the accretion should proceed via an NDAF rather than a CDAF in order for a significant amount of mass to reach the black hole. This condition imposes an upper limit on the radius of injection of the gas.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/aac6ad0d3edf985bac891eab1f3684cd2f9543f4

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In Astronomy and Astrophysics

1. Bing Zhang
2. B. Metzger
3. E. Berger
4. Pawan Kumar
5. E. Quataert
6. E. Nakar
7. D. Kasen
8. T. Piran

Citations in the corpus

• DISCERNING THE PHYSICAL ORIGINS OF COSMOLOGICAL GAMMA-RAY BURSTS BASED ON MULTIPLE OBSERVATIONAL CRITERIA: THE CASES OF z = 6.7 GRB 080913, z = 8.2 GRB 090423, AND SOME SHORT/HARD GRBs (2009, background): “…mergers (Paczýnski 1986; Eichler et al. 1989; Narayan et al. 1992; Rosswog et al. 2003), NS-BH mergers (Paczýnski 1991; Faber et al. 2006), and possibly BH-WD or NS-WD mergers (Fryer et al. 1999; King et al. 2007)(c.f. Narayan et al. 2001), see Nakar (2007); Lee & Ramirez-Ruiz (2007) for reviews.”
• Flares in Long and Short Gamma-Ray Bursts: A Common Origin in a Hyperaccreting Accretion Disk (2005, background): “…processes, are highly dependent on the mass accretion rate; for a given accretion rate, they further depend onthe radial location within the disk (e.g. Narayan et al. 2001; Di Matteo et al. 2002, DPN in the following) and on the composition which affects the opacity (Menou, Perna & Hernquist 2001).”
• Gamma-Ray Bursts in the Swift Era (2009, background): “…of forming NS and stellar– mass BHs during the collapse of massive stellar cores (Houck and Chevalier 1991, Woosley 1993, MacFadyen and Woosley 1999, Narayan et al. 2001) and in binary mergers involving compact objects (Ruffert et al. 1997, Kluzniak and Lee 1998, Rosswog and Liebendörfer 2003,…”
• The physics of gamma-ray bursts & relativistic jets (2014, methodology): “An approximate solution to the disk structure in the NDAF and ADAF regimes can be written in the following forms using results of numerical calculations [689,691,707,708,696,698]: NDAF:”
• Delayed outflows from black hole accretion tori following neutron star binary coalescence (2013, background): “However, the temperature is sufficiently high that neutrinos are relevant, especially in the earliest phases of the disk evolution (e.g., Popham et al. 1999; Narayan et al. 2001; Di Matteo et al. 2002; Chen & Beloborodov 2007; hereafter CB07).”
• Three-dimensional GRMHD Simulations of Neutrino-cooled Accretion Disks from Neutron Star Mergers (2017, background): “However, the disk can still be cooled by thermal neutrino emission (Popham et al. 1999; Narayan et al. 2001; Kohri & Mineshige 2002; Di Matteo et al. 2002; Beloborodov 2003; Kohri et al. 2005; Kawanaka & Mineshige 2007; Chen & Beloborodov 2007), a process that affects the lepton number of the disk…”
• The Supernova Gamma-Ray Burst Connection (2006, background): “Three possible mechanisms are discussed: 1) neutrinos (Woosley, 1993; Popham et al., 1999; Narayan et al., 2001; Di Matteo et al., 2002); 2) magnetic instabilities in the disk (Blandford and Payne, 1982; Proga et al., 2003); and 3) MHD extraction of the rotational energy of the black hole…”
• Long-term GRMHD simulations of neutron star merger accretion discs: implications for electromagnetic counterparts (2018, background): “Immediately after the merger, the disk is sufficiently hot and dense for neutrinos to be the primary cooling channel, with most of the nuclei fully dissociated into nucleons (Popham et al. 1999; Ruffert & Janka 1999; Narayan et al. 2001; Chen & Beloborodov 2007).”
• Time-dependent models of accretion discs formed from compact object mergers (2008, methodology): “This is the region most often modeled in previous studies (Popham et al. 1999; Narayan et al. 2001; Kohri & Mineshige 2002; DiMatteo et al. 2002; Chen & Beloborodov 2007).”
• General relativistic magnetohydrodynamic simulations of the jet formation and large-scale propagation from black hole accretion systems (2006, background): “An accretion disk is also formed as a result of a neutron star or black hole collisions with another stellar object (Narayan et al. 1992, 2001).”