Quantum Phase Transitions and the Failure of Classical General Relativity

Chapline, George

doi:10.1142/s0217751x03016380

Cited by 162 publications

(149 citation statements)

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“…In the model described in Chapline et al (2003), general relativity is an emergent theory of an underlying Lorentz violating microphysical theory, failing at small lengthscales. In this context, the gravastar is the result of a BEC-like phase transition induced by strong gravity.…”

Section: Accretion Heatingmentioning

confidence: 99%

Where are all the gravastars? Limits upon the gravastar model from accreting black holes

Broderick¹,

Narayan²

2007

Class. Quantum Grav.

104

112

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Abstract. The gravastar model, which postulates a strongly correlated thin shell of anisotropic matter surrounding a region of anti-de Sitter space, has been proposed as an alternative to black holes. We discuss constraints that present-day observations of well-known black hole candidates place on this model. We focus upon two black hole candidates known to have extraordinarily low luminosities: the supermassive black hole in the Galactic Center, Sagittarius A*, and the stellar-mass black hole, XTE J1118+480. We find that the length scale for modifications of the type discussed in Chapline et al. (2003)

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Section: Accretion Heatingmentioning

confidence: 99%

Where are all the gravastars? Limits upon the gravastar model from accreting black holes

Broderick¹,

Narayan²

2007

Class. Quantum Grav.

104

112

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“…The gravastar model assumes that the space-time undergoes a quantum vacuum phase transition in the vicinity of the BH horizon. The model effectively replaces the BH event horizon by a transition layer (or shell) and the BH interior by a segment of de Sitter space [33,34]. Mazur and Mottola argued for the thermodynamic stability of the model.…”

Section: Introductionmentioning

confidence: 99%

Gravitational wave signatures of the absence of an event horizon: Nonradial oscillations of a thin-shell gravastar

et al. 2009

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Gravitational waves from compact objects provide information about their structure, probing deep into strong-gravity regions. Here we illustrate how the presence or absence of an event horizon can produce qualitative differences in the gravitational waves emitted by ultracompact objects. In order to set up a straw-man ultracompact object with no event horizon, but which is otherwise almost identical to a black hole, we consider a nonrotating thin-shell model inspired by Mazur and Mottola's gravastar, which has a Schwarzschild exterior, a de Sitter interior and an infinitely thin shell with finite tension separating the two regions. As viewed from the external space-time, the shell can be located arbitrarily close to the Schwarzschild radius, so a gravastar might seem indistinguishable from a black hole when tests are only performed on its external metric. We study the linearized dynamics of the system, and, in particular, the junction conditions connecting internal and external gravitational perturbations. As a first application of the formalism we compute polar and axial oscillation modes of a thin-shell gravastar. We show that the quasinormal mode spectrum is completely different from that of a black hole, even in the limit when the surface redshift becomes infinite. Polar quasinormal modes depend on the equation of state of matter on the shell and can be used to distinguish between different gravastar models. Our calculations suggest that low-compactness gravastars could be unstable when the sound speed on the shell v s =c * 0:92.

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“…Black hole horizons introduce number of theoretical problems and a consensus of solutions of those problems has not yet been reached [2], [5].…”

Section: Introductionmentioning

confidence: 99%

“…In this scenario, quantum vacuum fluctuations are expected to play a non-trivial role in the collapse dynamics. A phase transition is believed to occur yielding a repulsive de Sitter core which helps balance the collapsing object thus preventing horizon (and singularity) formation [6], [5]. It is expected that this transition occurs very close to the limit 2m(r)/r = 1 so that, to an outside observer, it would be very difficult to distinguish the gravastar from a true black hole.…”

Section: Introductionmentioning

confidence: 99%