Ergoregion instability of ultracompact astrophysical objects
By V. Cardoso, Paolo Pani, Mariano Cadoni, Marco Cavaglià. 2007
139 citations recorded by the source corpus.
Most of the properties of black holes can be mimicked by horizonless compact objects such as gravastars and boson stars. We show that these ultracompact objects develop a strong ergoregion instability when rapidly spinning. Instability time scales can be of the order of 0.1 seconds to 1 week for objects with mass $M=1\ensuremath{-}{10}^{6}{M}_{\ensuremath{\bigodot}}$ and angular momentum $Jg0.4{M}^{2}$. This provides a strong indication that ultracompact objects with large rotation are black holes. Explosive events due to ergoregion instability have a well-defined gravitational-wave signature. These events could be detected by next-generation gravitational-wave detectors such as Advanced LIGO or LISA.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/fc8e42f5b3439c189c430ac55e8b508796fe8c14
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In Astronomy and Astrophysics
Citations in the corpus
- Dynamical boson stars (2012, background): “However, only fast spinning stars are subject to an ergoregion instability [84].”
- Superradiance: Energy Extraction, Black-Hole Bombs and Implications for Astrophysics and Particle Physics (2015, background): “This approach has been extended in subsequent work [392, 393, 394].”
- Tests for the existence of black holes through gravitational wave echoes (2017, background): “For ClePhOs, the ergoregioninstability timescale is parametrically longer than the dynamical timescale of the object [32, 34, 35].”
- Superradiance (2015, background): “ith subsequent work quantitatively describing the unstable modes for a scalar eld propagating on a slowly-rotating metric in the large-llimit [394]. This approach has been extended in subsequent work [395,396,397]. Most notably, Ref. [395] extended the analysis to the case of small multipoles (l;m),”
- Approximate Universal Relations for Neutron Stars and Quark Stars (2016, background): “[367] for slowly rotating gravastars and Chirenti and Rezzolla [368] for rapidly rotating gravastars.”
- Black holes in general relativity (2009, background): “For instance, rotating black hole mimics typically exhibit an ergoregion instability [56].”
- Numerical methods for finding stationary gravitational solutions (2015, unknown): “See [418, 469–473] for applications.”