Secular stellar dynamics near massive black holes

Details Secular stellar dynamics near massive black holes Secular stellar dynamics near massive black holes

Feb 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012phdt.........4m&link_type=abstract

Ph. D. thesis, University of Leiden (2012).

Physics

Black Hole Physics, Celestial Mechanics, Galaxy: Center, N-Body Simulations, Stellar Dynamics

Scientific paper

Stars near massive black holes move on elliptical orbits which precess slowly, exerting persistent gravitational torques on each other. In this the- sis we present four important consequences of these gravitational torques: 1) A new instability which exposes the inherently unstable nature of ec- centric stellar disks in galactic nuclei, 2) A density depression of stars near massive black holes due to enhanced angular momentum relaxation and tidal disruptions, 3) A signature of high-eccentricity orbits for stars formed by Hills' mechanism at large radii from the massive black hole, and a directly-observable statistic that can highlight these populations, and 4) A new dynamical process which we call "secular dynamical anti-friction" which boosts the orbital eccentricity of hypothesized intermediate-mass black holes as they spiral into massive black holes

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