The Fate of Nonradiative Magnetized Accretion Flows: Magnetically Frustrated Convection | Zendy

UeLi Pen | Zendy; Christopher D. Matzner | Zendy; Shingkwong Wong | Zendy

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The Fate of Nonradiative Magnetized Accretion Flows: Magnetically Frustrated Convection

Author(s) -

UeLi Pen,

Christopher D. Matzner,

Shingkwong Wong

Publication year - 2003

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/379339

Subject(s) - physics , accretion (finance) , polytrope , magnetohydrodynamics , convection , buoyancy , hydrostatic equilibrium , astrophysics , radius , accretion disc , mechanics , magnetic field , classical mechanics , astronomy , computer security , computer science , quantum mechanics , polytropic process

We present a scenario for non-radiative accretion onto the supermassive blackhole at the galactic center. Conducting MHD simulations with 1400^3 grid zonesthat break the axial and reflection symmetries of earlier investigations andextend inward from the Bondi radius, we find a quasi-hydrostatic radial densityprofile rho propto r^{-0.72} with superadiabatic gradient corresponding to ann~0.72 polytrope. Buoyancy generated by magnetic dissipation is resisted by thesame fields so effectively that energy is advected inward: a state ofmagnetically-frustrated convection. This scenario is consistent withobservational constraints on energetics andouter boundary conditions.Comment: 13 pages, 2 figures. Improved analysis of global flow energetics, implications, caveats, and relation to prior wor

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