Sphere of influence (black hole)

Short description: Region where a supermassive black hole gravitationally dominates its galaxy

The sphere of influence is a region around a supermassive black hole in which the gravitational potential of the black hole dominates the gravitational potential of the host galaxy. The radius of the sphere of influence is called the "(gravitational) influence radius".

There are two definitions in common use for the radius of the sphere of influence. The first[1] is given by rh=GMBHσ2 where MBH is the mass of the black hole, σ is the stellar velocity dispersion of the host bulge, and G is the gravitational constant.

The second definition[2] is the radius at which the enclosed mass in stars equals twice MBH, i.e. M⋆(r<rh)=2MBH.

Which definition is most appropriate depends on the physical question that is being addressed. The first definition takes into account the bulge's overall effect on the motion of a star, since σ is determined in part by stars that have moved far from the black hole. The second definition compares the force from the black hole to the local force from the stars.

It is a minimum requirement that the sphere of influence be well resolved in order that the mass of the black hole be determined dynamically.[3]

## Rotational influence sphere

If the black hole is rotating, there is a second radius of influence associated with the rotation.[4] This is the radius inside of which the Lense-Thirring torques from the black hole are larger than the Newtonian torques between stars. Inside the rotational influence sphere, stellar orbits precess at approximately the Lense-Thirring rate; while outside this sphere, orbits evolve predominantly in response to perturbations from stars on other orbits. Assuming that the Milky Way black hole is maximally rotating, its rotational influence radius is about 0.001 parsec,[5] while its radius of gravitational influence is about 3 parsecs.

## See also

* Roche limit
* Tidal disruption event § Tidal-disruption radius

## References

1. ↑ Peebles, J. (December 1972). "Star Distribution Near a Collapsed Object". The Astrophysical Journal 178: 371–376. doi:10.1086/151797. Bibcode: 1972ApJ...178..371P.
2. ↑ Merritt, David (2004). "Single and Binary Black Holes and their Influence on Nuclear Structure". in Ho, Luis. Coevolution of Black Holes and Galaxies. Carnegie Observatories Astrophysics Series. 1. Cambridge University Press. pp. 263–275. Bibcode: 2004cbhg.symp..263M. http://www.cambridge.org/us/catalogue/catalogue.asp?isbn=0521824494#contributors.
3. ↑ Ferrarese, Laura; Ford, Holland (2005). "Supermassive Black Holes in Galactic Nuclei: Past, Present and Future Research". Space Science Reviews 116 (3–4): 523–624. doi:10.1007/s11214-005-3947-6. Bibcode: 2005SSRv..116..523F.
4. ↑ Merritt, D. (2013). Dynamics and Evolution of Galactic Nuclei. Princeton, NJ: Princeton University Press. p. 284. ISBN 9781400846122. https://openlibrary.org/works/OL16802359W/Dynamics_and_Evolution_of_Galactic_Nuclei.
5. ↑ Merritt, David; Alexander, Tal; Mikkola, Seppo; Will, Clifford (2010). "Testing properties of the Galactic center black hole using stellar orbits". Physical Review D 81 (6): 062002. doi:10.1103/PhysRevD.81.062002. Bibcode: 2010PhRvD..81f2002M.

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