2007/02/23 by Norita Kawanaka, N. Kawanaka, Shin Mineshige +1 · 82 citations
Physics and Astronomy · #Accretion (finance) #Accretion disc #Astrophysical Phenomena and Observations #Astrophysics and Cosmic Phenomena #Astrophysics and Star Formation Studies #Inflow #Intermediate polar #Magnetorotational instability #Neutrino #Thermal #astro-ph
paper · pdf · doi:10.1086/517985
published in The Astrophysical Journal 662(2), 1156-1166 (IOP Publishing) · 26 pages, 28 figures, Accepted for publication in ApJ
arxiv created 2007/02/23 · openalex publication_date 2007/06/12 · arxiv updated 2011/02/11 · openalex created_date 2019/06/27 · openalex updated_date 2026/08/05
We investigate the structure and stability of hypercritical accretion flows around stellar-mass black holes, taking into account neutrino cooling, lepton conservation, and using for the first time a realistic equation of state in order to properly treat the dissociation of nuclei. We obtain the radial distributions of physical properties, such as density, temperature, and electron fraction, for various mass accretion rates 0.1-10 M ☉ s -1 . We find that, depending on mass accretion rates, different physics considerably affect the structure of the disk; the most important physics are (1) the photodissociation of nuclei around r ~ 100 r g for relatively low mass accretion rates ( ~ 0.01-0.1 M ☉ s -1 ), (2) efficient neutrino cooling around r ~ 10 r g -100 r g for moderately high mass accretion rates ( ~ 0.2-1.0 M ☉ s -1 ), and (3) neutrino trapping ( r ~ 3 r g -10 r g ) for very high mass accretion rates ( ≳ 2.0 M ☉ s -1 ). We also investigate the stability of hypercritical accretion flows by drawing the thermal equilibrium curves and find that efficient neutrino cooling makes the accretion flows rather stable against both thermal and viscous modes.