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Article overview
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Efficiency of Super-Eddington Magnetically-Arrested Accretion | | Jonathan C. McKinney
; Lixin Dai
; Mark Avara
; | | Date: |
10 Aug 2015 | | Abstract: | The radiative efficiency of super-Eddington accreting black holes (BHs) is
explored for magnetically-arrested disks (MADs), where magnetic flux builds-up
to saturation near the BH. Our three-dimensional general relativistic radiation
magnetohydrodynamic (GRRMHD) simulation of a spinning BH (spin $a/M=0.8$)
accreting at $sim 50$ times Eddington shows a total efficiency $sim 50\%$
when time-averaged and total efficiency $gtrsim 100\%$ in moments. Magnetic
compression by the magnetic flux near the rotating BH leads to a thin disk,
whose radiation escapes via advection by a magnetized wind and via transport
through a low-density channel created by a Blandford-Znajek (BZ) jet. The BZ
efficiency is sub-optimal due to inertial loading of field lines by optically
thick radiation, leading to BZ efficiency $sim 40\%$ on the horizon and BZ
efficiency $sim 5\%$ by $rsim 400r_g$ (gravitational radii) via absorption by
the wind. Importantly, radiation escapes at $rsim 400r_g$ with efficiency
$etaapprox 15\%$ (luminosity $Lsim 50L_{
m Edd}$), similar to $etaapprox
12\%$ for a Novikov-Thorne thin disk and beyond $etalesssim 1\%$ seen in
prior GRRMHD simulations or slim disk theory. Our simulations show how BH spin,
magnetic field, and jet mass-loading affect the radiative and jet efficiencies
of super-Eddington accretion. | | Source: | arXiv, 1508.2433 | | Services: | Forum | Review | PDF | Favorites | |
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