Orbits Around Black Holes in Triaxial Nuclei

@article{Merritt2011OrbitsAB,
  title={Orbits Around Black Holes in Triaxial Nuclei},
  author={David Merritt and Eugene Vasiliev},
  journal={The Astrophysical Journal},
  year={2011},
  volume={726},
  pages={61}
}
We discuss the properties of orbits within the influence sphere of a supermassive black hole (BH), in the case that the surrounding star cluster is non-axisymmetric. There are four major orbit families; one of these, the pyramid orbits, have the interesting property that they can approach arbitrarily closely to the BH. We derive the orbit-averaged equations of motion and show that in the limit of weak triaxiality, the pyramid orbits are integrable: the motion consists of a two-dimensional… Expand
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References

SHOWING 1-10 OF 43 REFERENCES
Stellar Orbits in Triaxial Clusters around Black Holes in Galactic Nuclei
We investigate the orbital structure of a model triaxial star cluster, centered around a supermassive black hole (BH), appropriate to galactic nuclei. Sridhar & Touma proved in 1999 that the presenceExpand
Orbital Structure of Triaxial Black Hole Nuclei
Orbital motion in triaxial nuclei with central point masses, representing supermassive black holes, is investigated. The stellar density is assumed to follow a power law ρ ∝ r-γ, with γ = 1 or γ = 2.Expand
Stellar dynamics around black holes in galactic nuclei
We classify orbits of stars that are bound to central black holes in galactic nuclei. The stars move under the combined gravitational influences of the black hole and the central star cluster. WithinExpand
A self-consistent study of triaxial black-hole nuclei
We construct models of triaxial galactic nuclei containing central black holes using the method of orbital superposition and then verify their stability by advancing N-body realizations of the modelsExpand
Resonant Orbits in Triaxial Galaxies
Box orbits in triaxial potentials are generically thin, that is, they lie close in phase space to a resonant orbit satisfying a relation of the form lω1 + mω2 + nω3 = 0 between the three fundamentalExpand
Gravitational loss-cone instability in stellar systems with retrograde orbit precession
We study spherical and disc clusters in a near-Keplerian potential of galactic centres or massive black holes. In such a potential orbit precession is commonly retrograde, that is, the direction ofExpand
The tidal disruption rate in dense galactic cusps containing a supermassive binary black hole
We consider the problem of tidal disruption of stars in the centre of a galaxy containing a supermassive binary black hole with unequal masses. We assume that over the separation distance between theExpand
Testing properties of the Galactic center black hole using stellar orbits
The spin and quadrupole moment of the supermassive black hole at the Galactic center can in principle be measured via astrometric monitoring of stars orbiting at milliparsec distances, allowing testsExpand
Resonant Relaxation near a Massive Black Hole: The Stellar Distribution and Gravitational Wave Sources
Resonant relaxation (RR) of orbital angular momenta occurs near massive black holes (MBHs) where the potential is spherical and stellar orbits are nearly Keplerian and so do not precessExpand
CHAOTIC LOSS CONES AND BLACK HOLE FUELING
In classical loss cone theory, stars are supplied to a central black hole via gravitational scattering onto low angular momentum orbits. Higher feeding rates are possible if the gravitationalExpand
...
1
2
3
4
5
...