The Fate of Non-Radiative Magnetized Accretion Flows: Magnetically-Frustrated Convection

Details The Fate of Non-Radiative Magnetized Accretion Flows: Magnetically-Frustrated Convection The Fate of Non-Radiative Magnetized Accretion Flows: Magnetically-Frustrated Convection

2003-04-12

arxiv.org/abs/astro-ph/0304227v3

Astrophys.J. 596 (2003) L207-L210

Astronomy and Astrophysics

Astrophysics

13 pages, 2 figures. Improved analysis of global flow energetics, implications, caveats, and relation to prior work

Scientific paper

10.1086/379339

We present a scenario for non-radiative accretion onto the supermassive black hole at the galactic center. Conducting MHD simulations with 1400^3 grid zones that break the axial and reflection symmetries of earlier investigations and extend inward from the Bondi radius, we find a quasi-hydrostatic radial density profile rho propto r^{-0.72} with superadiabatic gradient corresponding to an n~0.72 polytrope. Buoyancy generated by magnetic dissipation is resisted by the same fields so effectively that energy is advected inward: a state of magnetically-frustrated convection. This scenario is consistent with observational constraints on energetics andouter boundary conditions.

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