How to tell a gravastar from a black hole
By C. Chirenti, Luciano Rezzolla. 2007
236 citations recorded by the source corpus.
Gravastars have been recently proposed as potential alternatives to explain the astrophysical phenomenology traditionally associated with black holes, raising the question of whether the two objects can be distinguished at all. Leaving aside the debate about the processes that would lead to the formation of a gravastar and the astronomical evidence in their support, here we address two basic questions: is a gravastar stable against generic perturbations? If it is stable, can an observer distinguish it from a black hole of the same mass? To answer these questions we construct a general class of gravastars and determine the conditions they must satisfy in order to exist as equilibrium solutions of the Einstein equations. For such models we perform a systematic stability analysis against axial perturbations, computing the real and imaginary parts of the eigenfrequencies. Overall, we find that gravastars are stable to axial perturbations, but also that their quasi-normal modes differ from those of a black hole of the same mass and thus can be used to discern, beyond dispute, a gravastar from a black hole.
View Paper: https://www.semanticscholar.org/paper/1a755adfaeb9156f86acffece196534fcb098907
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Citations in the corpus
- Regular Black Holes with Asymptotically Minkowski Cores (2019, background): “[3–7]) regular black holes, but also the Mazur–Mottola gravastars [8–16], and Dymnikova’s models [17–21].”
- A coordinate-independent characterization of a black hole shadow (2015, background): “…to justify a lack of emission from such a surface (Broderick & Narayan 2007); gravitational-wave emission would unambiguously signal the presence of an event horizon (Chirenti & Rezzolla 2007). will fall down into the event horizon, while photons circling just outside will escape to infinity.”
- Approximate Universal Relations for Neutron Stars and Quark Stars (2016, background): “interesting to study the I-Love-Q relations for other gravastar models, such as those with a finite-thickness boundary layer [359, 368], with the interior region supported by dark energy instead of a cosmological constant (phantom gravastars or dark energy stars) [379, 380].”
- Superradiance: Energy Extraction, Black-Hole Bombs and Implications for Astrophysics and Particle Physics (2015, background): “In the static case these models have been shown to be thermodynamically [398] and dynamically [537, 538, 531] stable for reasonable equations of state.”
- Shadows of spherically symmetric black holes and naked singularities (2018, unknown): “(21) of Chirenti & Rezzolla 2007), p′r = −(ρ + pr ) m(r) + r3pr/2 r(r − 2m(r)) + 2 r (pθ − pr ), (10) where we have set 8πG = 1 and c = 1, and gi (r) = 1 − 2m(r) r , 2m(r) = ∫ r 0 ρr2dr .”
- Superradiance (2015, background): “sure of the de Sitter interior contributes to sustain the self-gravity of the object for any compactness. In the static case these models have been shown to be thermodynamically [401] and dynamically [541,542,535] stable for reasonable equations of state. Superspinars are BH-like objects described b”