Neutrino-Cooled Accretion Disks around Spinning Black Hole
| dc.creator | Chen, Wen-Xin | |
| dc.creator | Beloborodov, Andrei M. | |
| dc.date | 2006-07-07 | |
| dc.date | 2006-07-17 | |
| dc.date.accessioned | 2026-07-07T10:23:17Z | |
| dc.date.available | 2026-07-07T10:23:17Z | |
| dc.description | We calculate the structure of accretion disks around Kerr black holes for accretion rates 0.001 - 10 M_sun/s. Such disks are plausible candidates for the central engine of gamma-ray bursts. Our disk model is fully relativistic and treats accurately microphysics of the accreting matter: neutrino emissivity, opacity, electron degeneracy, and nuclear composition. The neutrino-cooled disk forms above a critical accretion rate that depends on the black hole spin. The disk has the ``ignition'' radius r_ign where neutrino flux rises dramatically, cooling becomes efficient, and the proton-to-nucleon ratio Y_e drops. Other characteristic radii are r_alpha where most of alpha-particles are disintegrated, r_nu where the disk becomes neutrino-opaque, and r_trap where neutrinos get trapped and advected into the black hole. We find r_alpha, r_ign, r_nu, r_trap and show their dependence on the accretion rate. We discuss the qualitative picture of accretion and present sample numerical models of the disk structure. All neutrino-cooled disks regulate themselves to a characteristic state such that: (1) electrons are mildly degenerate, (2) Y_e ~ 0.1, and (3) neutrons dominate the pressure in the disk. | |
| dc.description | 35 pages, 18 figures, accepted to ApJ | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0607145 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0607145 | |
| dc.identifier | Astrophys.J.657:383-399,2007 | |
| dc.identifier | doi:10.1086/508923 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/175775 | |
| dc.subject | Astrophysics | |
| dc.title | Neutrino-Cooled Accretion Disks around Spinning Black Hole | |
| dc.type | text |