2002
DOI: 10.1086/338077
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Three‐dimensional Magnetohydrodynamic Simulations of Spherical Accretion

Abstract: We present three-dimensional numerical magnetohydrodynamic simulations of radiatively inefficient spherical accretion onto a black hole. The simulations are initialized with a Bondi Ñow and with a weak, dynamically unimportant, large-scale magnetic Ðeld. As the gas Ñows in, the magnetic Ðeld is ampliÐed. When the magnetic pressure approaches equipartition with the gas pressure, the Ðeld begins to reconnect and the gas is heated up. The heated gas is buoyant and moves outward, causing line stretching of the fro… Show more

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Cited by 91 publications
(106 citation statements)
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“…Note that even for spherical accretion (i.e., in the absence of differential rotation and the MRI ), a significant fraction of the gravitational potential energy of the inflowing gas may be converted into heat. In particular, even initially weak magnetic fields are compressed by flux freezing until they become strong, leading to reconnection and significant heating (Igumenshchev & Narayan 2002). Because v e 3 v i unless T e P10 À3 T i , electron heat conduction tends to be more important than ion heat conduction.…”
Section: Energy Equationsmentioning
confidence: 99%
“…Note that even for spherical accretion (i.e., in the absence of differential rotation and the MRI ), a significant fraction of the gravitational potential energy of the inflowing gas may be converted into heat. In particular, even initially weak magnetic fields are compressed by flux freezing until they become strong, leading to reconnection and significant heating (Igumenshchev & Narayan 2002). Because v e 3 v i unless T e P10 À3 T i , electron heat conduction tends to be more important than ion heat conduction.…”
Section: Energy Equationsmentioning
confidence: 99%
“…The stability of the b-h flow was put into question with numerical results glimpsing various instabilities without being able to agree whether their origin was physical or not (see Foglizzo et al 2005, and references therein). Meanwhile, analytical progresses were also made as physical effects were added or coupled together : small or large scale magnetic fields (Igumenshchev and Narayan 2002;Igumenshchev 2006;Pang et al 2011), net vorticity (Krumholz et al 2005), radiative feedback (Park and Ricotti 2013), finite size accretors (Ruffert 1994a), turbulence (Krumholz et al 2006), etc. Simulations of accretion onto not compact objects like stars orbiting an agb companion in a symbiotic binary (Theuns et al 1996;de Val-Borro et al 2009) have deeply improved our understanding of the barium enriched stars (Bidelman and Keenan 1951) ; but the wide dynamics introduced by the small size of a compact object compared to its gravitational sphere of influence on non-relativistic winds has prevented numerical simulations to converge to a b-h accretion solution around a compact object up to now.…”
Section: Introductionmentioning
confidence: 99%
“…If the outflow is strong enough, then the amount of mass reaching the BH could be a great deal less than the mass supplied on the outside [107], [108] (but see [109], [110]). [105]. Note the obvious turbulent eddies which are due to convection.…”
Section: Convection-dominated Accretion Flow (Cdaf)mentioning
confidence: 98%
“…The density profile of a magnetized spherical flow was found to differ significantly from the R −3/2 behavior predicted by the Bondi model ( §4), and the mass accretion rate was found to be much less than the value given in (2). The reason for the discrepancy is as follows [105].…”
Section: Bondi Accretion With Magnetic Fieldsmentioning
confidence: 99%