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Direct imaging rapidly-rotating non-Kerr black holes

MPG-Autoren

Caravelli,  Francesco
Microscopic Quantum Structure & Dynamics of Spacetime, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Volltexte (frei zugänglich)

1110.2768
(Preprint), 679KB

PLB711_10.pdf
(beliebiger Volltext), 427KB

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Zitation

Bambi, C., Caravelli, F., & Modesto, L. (2012). Direct imaging rapidly-rotating non-Kerr black holes. Physics Letters B, 711, 10-14. doi:10.1016/j.physletb.2012.03.068.


Zitierlink: http://hdl.handle.net/11858/00-001M-0000-000E-EE85-1
Zusammenfassung
Recently, two of us have argued that non-Kerr black holes in gravity theories different from General Relativity may have a topologically non-trivial event horizon. More precisely, the spatial topology of the horizon of non-rotating and slow-rotating objects would be a 2-sphere, like in Kerr space-time, while it would change above a critical value of the spin parameter. When the topology of the horizon changes, the black hole central singularity shows up. The accretion process from a thin disk can potentially overspin these black holes and induce the topology transition, violating the Weak Cosmic Censorship Conjecture. If the astrophysical black hole candidates are not the black holes predicted by General Relativity, we might have the quite unique opportunity to see their central region, where classical physics breaks down and quantum gravity effects should appear. Even if the quantum gravity region turned out to be extremely small, at the level of the Planck scale, the size of its apparent image would be finite and potentially observable with future facilities.