Can Neutrino-cooled Accretion Disks Be an Origin of Gamma-Ray Bursts?

By K. Kohri, S. Mineshige. 2002

167 citations recorded by the source corpus.

It is often proposed that a massive torus with approximately solar mass surrounding a stellar-mass black hole could be a central engine of gamma-ray bursts. We study the properties of such massive accretion tori (or disks) based on the α viscosity model. For surface density exceeding about 1020 g cm-2, which is realized when ~1 M☉ of material is contained within a disk of size ~5 × 106 cm, we find that (1) the luminosity of photons is practically zero because of significant photon trapping, (2) neutrino cooling dominates over advective cooling, (3) the pressure of degenerate electrons dominates over the pressure of gas and photons, and (4) the magnetic field strength exceeds the critical value of about 4 × 1013 G, even if we take 0.1% of the equipartition value. The possible observable quantum electrodynamical (QED) effects arising from supercritical fields are discussed. Most interestingly, photon splitting may occur, producing a significant number of photons of energies below ~511 keV, thereby possibly suppressing e± pair creation.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/fc0b224d5fabd653e874f019fbe40920cadaafc0

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In Astronomy and Astrophysics

1. B. Metzger
2. Bing Zhang
3. E. Quataert
4. Pawan Kumar
5. E. Nakar
6. J. McKinney
7. Ramesh Narayan
8. T. Piran

Citations in the corpus

• Comprehensive nucleosynthesis analysis for ejecta of compact binary mergers (2014, background): “…the tori cool predominantly by neutrino emission while photons are trapped and contribute to the pressure as a plasma component in thermal equilibrium with electrons, positrons, nucleons and nuclei (see, e.g. Popham et al. 1999; Di Matteo, Perna & Narayan 2002; Kohri & Mineshige 2002).”
• 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…”
• A Reconnection Switch to Trigger gamma-Ray Burst Jet Dissipation (2010, background): “We follow Kohri & Mineshige (2002) (see also Kohri et al. 2005), except their energy density loss rates assume that there exists an optically-thick thermalized photon and pair bath, while in this work the photon and pair densities are reduced by a factor of g[τ γ ] and g[τ pairs], respectively.”
• Neutrino-cooled Accretion Disks around Spinning Black Holes (2006, background): “Kohri & Mineshige (2002) studied strongly1 Also at: Astro Space Center, Lebedev Physical Institute, Moscow, Russia.”
• Neutrino-dominated accretion flows as the central engine of gamma-ray bursts (2017, background): “In another discussion, Kohri & Mineshige (2002) pointed out that electron degeneracy can suppress neutrino emission.”
• Neutrino-dominated Accretion and Supernovae (2005, methodology): “The model we employ for the calculations is more elaborate than those described in the recent literature (Popham et al. 1999; Narayan et al. 2001; Kohri & Mineshige 2002; Di Matteo et al. 2002), and we highlight the improvements.”
• Short-hard gamma-ray bursts (2007, background): “Considerations of the strong magnetic fields that might be present in hyper-accreting disk as well as observable quantum electrodynamical effects arising from supercritical fields are discussed by Kohri & Mineshige (2002).”
• Dynamical Evolution of Neutrino-cooled Accretion Disks: Detailed Microphysics, Lepton-driven Convection, and Global Energetics (2005, methodology): “Over the last several years, many groups have considered these cases in the neutrino cooled regime (Popham, Woosley & Fryer 1999; Narayan, Piran & Kumar 2001; Kohri & Mineshige 2002; DiMatteo, Perna & Narayan 2002; Yokosawa etl.”
• Equation of state in relativistic magnetohydrodynamics: variable versus constant adiabatic index (2007, background): “…for a combination of protons, neutrons, electrons, positrons, and neutrinos, etc. and must include the effects of electron degeneracy, neutronization, photodisintegration, optical depth of neutrinos, etc. (Popham et al. 1999; Di Matteo et al. 2002; Kohri & Mineshige 2002; Kohri et al. 2005).”
• The physics of gamma-ray bursts & relativistic jets (2014, unknown): “…the NDAF and ADAF regimes can be written in the following forms using results of numerical calculations (Popham et al., 1999; Narayan et al., 2001; Kohri and Mineshige, 2002; Kohri et al., 2005; Chen and Beloborodov, 2007; Yuan and Zhang, 2012): NDAF: ρ= 1.2× 1014 g cm−3 α−1.3−2 Ṁ−1 ( M 3M )−1.7…”
• 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, methodology): “The chosen H/R and the extent of the disk are similar to the accretion disk that is expected to form in the collapsar model (MacFadyen & Woosley 1999; Kohri & Mineshige 2002; Kohri et al. 2005).”
• Nuclear Composition of Gamma-Ray Burst Fireballs (2002, background): “The only cooling mechanism of the flow is neutrino emission, which becomes efficient at _Me1031 g s 1 and small r (e.g., Popham, Woosley, & Fryer 1999; Narayan, Piran, & Kumar 2001; Kohri & Mineshige 2002).”
• Mass fall-back and accretion in the central engine of gamma-ray bursts (2008, background): “A number of later investigators have studied the physics of these two regimes of accretion in the context of GRB models (Di Matteo, Perna & Narayan 2002; Kohri & Mineshige 2002; Janiuk et al. 2004, 2007; Lee, Ramirez-Ruiz & Page 2004, 2005; Kohri, Narayan & Piran 2005, and references therein).”
• Neutrino Trapping and Accretion Models for Gamma-Ray Bursts (2002, methodology): “Accretion models in the context of GRBs have been recently discussed by Popham, Woosley & Fryer (1999; hereafter PWF), Narayan, Piran & Kumar (2001; hereafter NPK) and Kohri & Mineshige (2002).”