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#### The slicing dependence of non-spherically symmetric quasi-local horizons in Vaidya Spacetimes

##### MPG-Autoren
http://pubman.mpdl.mpg.de/cone/persons/resource/persons4362

Jasiulek,  Michael
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

http://pubman.mpdl.mpg.de/cone/persons/resource/persons20661

Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

##### Externe Ressourcen
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##### Volltexte (frei zugänglich)

1007.2990
(Preprint), 202KB

PRD83_124022.pdf
(beliebiger Volltext), 572KB

##### Ergänzendes Material (frei zugänglich)
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##### Zitation

Nielsen, A. B., Jasiulek, M., Krishnan, B., & Schnetter, E. (2011). The slicing dependence of non-spherically symmetric quasi-local horizons in Vaidya Spacetimes. Physical Review D, 83(12): 124022. doi:10.1103/PhysRevD.83.124022.

It is well known that quasi-local black hole horizons depend on the choice of a time coordinate in a spacetime. This has implications for notions such as the surface of the black hole and also on quasi-local physical quantities such as horizon measures of mass and angular momentum. In this paper, we compare different horizons on non-spherically symmetric slicings of Vaidya spacetimes. The spacetimes we investigate include both accreting and evaporating black holes. For some simple choices of the Vaidya mass function function corresponding to collapse of a hollow shell, we compare the area for the numerically found axisymmetric trapping horizons with the area of the spherically symmetric trapping horizon and event horizon. We find that as expected, both the location and area are dependent on the choice of foliation. However, the area variation is not large, of order $0.035\%$ for a slowly evolving horizon with $\dot{m}=0.02$. We also calculate analytically the difference in area between the spherically symmetric quasi-local horizon and event horizon for a slowly accreting black hole. We find that the difference can be many orders of magnitude larger than the Planck area for sufficiently large black holes.