Resonant relaxation near a massive black hole: the dependence on eccentricity

Details Resonant relaxation near a massive black hole: the dependence on eccentricity Resonant relaxation near a massive black hole: the dependence on eccentricity

2007-04-20

arxiv.org/abs/0704.2709v1

Mon.Not.Roy.Astron.Soc.379:1083-1088,2007

Astronomy and Astrophysics

Astrophysics

6 pages, 5 figures, submitted to MNRAS main journal

Scientific paper

10.1111/j.1365-2966.2007.11982.x

The orbits of stars close to a massive black hole are nearly Keplerian ellipses. Such orbits exert long term torques on each other, which lead to an enhanced angular momentum relaxation known as resonant relaxation. Under certain conditions, this process can modify the angular momentum distribution and affect the interaction rates of the stars with the massive black hole more efficiently than non-resonant relaxation. The torque on an orbit exerted by the cluster depends on the eccentricity of the orbit. In this paper, we calculate this dependence and determine the resonant relaxation timescale as a function of eccentricity. In particular, we show that the component of the torque that changes the magnitude of the angular momentum is linearly proportional to eccentricity, so resonant relaxation is much more efficient on eccentric orbits than on circular orbits.

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