A Magnetohydrodynamic Nonradiative Accretion Flow in Three Dimensions

By J. Hawley, Steven Balbus, James M. Stone. 2001

133 citations recorded by the source corpus.

We present a global magnetohydrodynamic (MHD) three-dimensional simulation of a nonradiative accretion flow originating in a pressure-supported torus. The evolution is controlled by the magnetorotational instability, which produces turbulence. The flow forms a nearly Keplerian disk. The total pressure scale height in this disk is comparable to the vertical size of the initial torus. Gas pressure dominates near the equator; magnetic pressure is more important in the surrounding atmosphere. A magnetically dominated bound outflow is driven from the disk. The accretion rate through the disk exceeds the final rate into the hole, and a hot torus forms inside 10rg. Hot gas, pushed up against the centrifugal barrier and confined by magnetic pressure, is ejected in a narrow, unbound, conical outflow. The dynamics are controlled by magnetic turbulence, not thermal convection, and a hydrodynamic α-model is inadequate to describe the flow. The limitations of two-dimensional MHD simulations are also discussed.

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Citations in the corpus

The Dynamical Structure of Nonradiative Black Hole Accretion Flows (2002, background): “Marginal stability to the classical Høiland criteria is not achieved, nor could it be achieved as a matter of principle (Hawley et al. 2001).”
Electron Heating in Hot Accretion Flows (2007, methodology): “GlobalMHD simulations support the former possibility (Stone & Pringle 2001; Hawley et al. 2001).”
Three-dimensional Magnetohydrodynamic Simulations of Radiatively Inefficient Accretion Flows (2003, background): “Hawley et al. (2001) and Hawley & Balbus (2002) have carried out three-dimensional MHD simulations of rotating flows but do not see any evidence for field accumulation at the center.”
Stability of relativistic jets from rotating, accreting black holes via fully three-dimensional magnetohydrodynamic simulations (2008, background): “…et al. 2008) to injecting a jet from an unresolved Keplerian disc (e.g., Tchekhovskoy et al. 2008), and to evolving both the disc and jet (e.g., Hawley et al. 2001; McKinney & Gammie 2002, 2004; Kigure & Shibata 2005; McKinney 2005; Hawley & Krolik 2006; McKinney 2006a; McKinney & Narayan…”
Hot Accretion Flows Around Black Holes (2014, background): “…hydro simulations (Stone et al. 1999, Yuan & Bu 2010, Yuan et al. 2012b, Li et al. 2013a) or MHD simulations (Stone & Pringle 2001, Machida et al. 2001, Hawley et al. 2001, Hawley & Balbus 2002, Igumenshchev et al. 2003, Pen et al. 2003, Kato et al. 2004b, Pang et al. 2011, Yuan et al. 2012a).”
Three-dimensional general relativistic radiation magnetohydrodynamical simulation of super-Eddington accretion, using a new code HARMRAD with M1 closure (2013, background): “…& Blandford 2009) and |H/R| ∼ 0.3–0.4 (Igumenshchev et al. 2003; Penna et al. 2010), as well as radiatively efficient, geometrically thick flows with |H/R| ∼ 0.6–1.0 (Stone & Pringle 2001; Hawley et al. 2001; Igumenshchev & Narayan 2002; Pen et al. 2003; Pang et al. 2011; McKinney et al. 2012).”
General relativistic magnetohydrodynamic simulations of magnetically choked accretion flows around black holes (2012, unknown): “…2003; McKinney & Gammie 2004; Fragile et al. 2007; McKinney & Blandford 2009), |H/R| ∼ 0.3–0.4 (Igumenshchev et al. 2003; Penna et al. 2010), |H/R| ∼ 0.6 (Run F type in Stone & Pringle 2001; Hawley et al. 2001), and rarely |H/R| ∼ 1 (Igumenshchev & Narayan 2002; Pen et al. 2003; Pang et al. 2011).”