Radiative Efficiency of Collisionless Accretion

Details Radiative Efficiency of Collisionless Accretion Radiative Efficiency of Collisionless Accretion

1997-10-13

arxiv.org/abs/astro-ph/9710132v1

Astrophys.J. 501 (1998) 787

Astronomy and Astrophysics

Astrophysics

12 pages, Latex, Submitted to ApJ

Scientific paper

10.1086/305845

Radiative efficiency of a slowly accreting black hole is estimated using a two-temperature model of accretion. The radiative efficiency depends on the magnetic field strength near the Schwarzschild radius. For weak magnetic fields (magnetic energy=equipartition/1000), the low efficiency 0.0001 assumed in some theoretical models might be achieved. For stronger fields, a significant fraction of viscous heat is dissipated by electrons and radiated away resulting in a larger efficiency. At equipartition magnetic fields, we estimate efficiency = of order 10%.

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