Radiative Efficiency of Collisionless Accretion
Astrophysics
2009-10-30 v1
Abstract
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%.
Cite
@article{arxiv.astro-ph/9710132,
title = {Radiative Efficiency of Collisionless Accretion},
author = {Andrei V. Gruzinov},
journal= {arXiv preprint arXiv:astro-ph/9710132},
year = {2009}
}
Comments
12 pages, Latex, Submitted to ApJ