Neutrino Trapping and Accretion Models for Gamma-Ray Bursts

By T. Di Matteo, R. Perna, Ramesh Narayan. 2002

275 citations recorded by the source corpus.

Many models of gamma-ray bursts (GRBs) invoke a central engine consisting of a black hole of a few solar masses accreting matter from a disk at a rate of a fraction to a few solar masses per second. Popham et al. and Narayan et al. have shown that, for Ṁ≳ 0.1 M☉ s-1, accretion proceeds via neutrino cooling and neutrinos can carry away a significant amount of energy from the inner regions of the disks. We improve on these calculations by including a simple prescription for neutrino transfer and neutrino opacities in such regions. We find that the flows become optically thick to neutrinos inside a radius R ~ 6RS-40RS for Ṁ in the range of 0.1-10 M☉ s-1, where RS is the black hole Schwarzchild radius. Most of the neutrino emission comes from outside this region, and the neutrino luminosity stays roughly constant at a value Lν ~ 1053 ergs s-1. We show that, for Ṁ ≳ 1 M☉ s-1, neutrinos are sufficiently trapped that energy advection becomes the dominant cooling mechanism in the flow. These results imply that νν̄ annihilation in hyperaccreting black holes is an inefficient mechanism for liberating large amounts of energy. Extraction of rotational energy by magnetic processes remains the most viable mechanism.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/67ca95e5a731b1008b830976617a6c8d5f53dc3f

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Citations in the corpus

Magnetic acceleration of ultrarelativistic jets in gamma-ray burst sources (2008, result): “Although this model remains very popular, some recent studies have indicated that the neutrino heating may not be as efficient as previously thought (e.g. Di Matteo et al. 2002).”
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…”
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…”
Neutrino-dominated accretion flows as the central engine of gamma-ray bursts (2017, methodology): “The cooling rate due to neutrino loss Qν is expressed in accordance to the above bridging formula of uν (e.g., Di Matteo et al. 2002; Kohri et al. 2005; Liu et al. 2007; Xue et al. 2013), Qν = ∑ i (7/8)σT 4 (3/4)[τνi/2 + 1/ √ 3 + 1/(3τa,νi)] .”
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, background): “…these requirements: a hyper-accreting stellar-mass black hole (Woosley, 1993; Popham et al., 1999; Lee et al., 2000; Narayan et al., 2001; Di Matteo et al., 2002; Wang et al., 2002; McKinney, 2005; Uzdensky and MacFadyen, 2006; Chen and Beloborodov, 2007; Lei et al., 2009, 2013; Yuan and…”
Delayed outflows from black hole accretion tori following neutron star binary coalescence (2013, background): “In this case cs ≃ (4kBT/3mp)1/2 and κν ≃ κ0T 2 (where κ0 ≃ 4.5 × 10−39 K−2cm2g−1; e.g. Di Matteo et al. 2002).”
Neutrino-cooled Accretion Disks around Spinning Black Holes (2006, background): “For example, Di Matteo et al. (2002) focused on the effects of neutrino opacity at high Ṁ ; however they neglected degeneracy and assumed nn/np ¼ 1.”