Built on

E. T. Newman and A. I. Janis, Journal of Mathematical Physics 6
1965
Earlier work this paper cites.
R. P. Geroch, J.Math.Phys. 11
1970
Earlier work this paper cites.
R. Hansen, J.Math.Phys. 15
1974
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S. Chandrasekhar, The mathematical theory of black holes (1983)
1983
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S. Mignemi and N. Stewart, Phys.Rev. D47
1993
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F. Ryan, Phys.Rev. D52
1995
Earlier work this paper cites.
N. A. Collins and S. A. Hughes, Phys.Rev. D69
2004
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J. G. Williams, S. G. Turyshev, and D. H. Boggs, Phys.Rev.Lett. 93
2004
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K. Glampedakis and S. Babak, Class.Quant.Grav. 23
2006
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C. M. Will, Living Rev.Rel. 9
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F. Eisenhauer, G. Perrin, W. Brandner, C. Straubmeier, A. Richichi, et al. , (2008), arXiv:0808.0063 [astro-ph]
Original
2008
Earlier work this paper cites.
D. Psaltis, D. Perrodin, K. R. Dienes, and I. Mocioiu, Phys.Rev.Lett. 100
Original
2008
Earlier work this paper cites.

Similar

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Then

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Original
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Later among the works it cites.
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Original
2011
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Original
2012
Later among the works it cites.
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Original
2013
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2014

On generic parametrizations of spinning black-hole geometries

Cardoso, Vitor, Pani, Paolo, Rico, Joao

Understand

The construction of a generic parametrization of spinning geometries which can be matched continuously to the Kerr metric is an important open problem in General Relativity.

Its resolution is more than of academic interest, as it allows to parametrize and quantify possible deviations from the no-hair theorem.
Various approaches to the problem have been proposed, all with their own (severe) limitations.
Here we discuss the metric recently proposed by Johannsen and Psaltis, showing that (i) the original metric describes only corrections that preserve the horizon area-mass relation of nonspinning geometries; (ii) this unnecessary restriction can be relaxed by introducing a new parameter that in fact dominates in both the post-Newtonian and strong-field regimes; (iii) within this framework, we construct the most generic spinning black-hole geometry which contains twice as many the (infinite) parameters of the original metric; (iv) in the strong-field regime, all parameters are roughly equally important.

Built on

E. T. Newman and A. I. Janis, Journal of Mathematical Physics 6
1965
Earlier work this paper cites.
R. P. Geroch, J.Math.Phys. 11
1970
Earlier work this paper cites.
R. Hansen, J.Math.Phys. 15
1974
Earlier work this paper cites.
S. Chandrasekhar, The mathematical theory of black holes (1983)
1983
Earlier work this paper cites.
S. Mignemi and N. Stewart, Phys.Rev. D47
1993
Earlier work this paper cites.
F. Ryan, Phys.Rev. D52
1995
Earlier work this paper cites.
N. A. Collins and S. A. Hughes, Phys.Rev. D69
2004
Earlier work this paper cites.
J. G. Williams, S. G. Turyshev, and D. H. Boggs, Phys.Rev.Lett. 93
2004
Earlier work this paper cites.
K. Glampedakis and S. Babak, Class.Quant.Grav. 23
2006
Earlier work this paper cites.
C. M. Will, Living Rev.Rel. 9
2006
Earlier work this paper cites.
F. Eisenhauer, G. Perrin, W. Brandner, C. Straubmeier, A. Richichi, et al. , (2008), arXiv:0808.0063 [astro-ph]
Original
2008
Earlier work this paper cites.
D. Psaltis, D. Perrodin, K. R. Dienes, and I. Mocioiu, Phys.Rev.Lett. 100
Original
2008
Earlier work this paper cites.