Evolution of 3D boson stars with waveform extraction

Balakrishna, Jayashree; Bondarescu, Ruxandra; Daues, Gregory; Guzmán, F. S.; Seidel, Edward

doi:10.1088/0264-9381/23/7/024

Cited by 45 publications

(51 citation statements)

References 54 publications

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“…They computed the dominant axial oscillation modes and found no instabilities. In analogy with previous studies of the oscillation modes of boson stars [29][30][31], they confirmed that the axial QNM spectrum of gravastars can be used to discern a gravastar from a BH. In the thin-shell limit, the axial QNM frequencies of Ref.…”

Section: Introductionsupporting

confidence: 82%

“…Building on Ryan's proposal, Kesden et al showed that the inspiral of a small compact object into a nonrotating boson star will emit a rather different gravitational waveform at the end of the evolution, when the small object falls into the central potential well of the boson star instead of disappearing into the event horizon of a BH [28]. Several authors have computed the QNM spectrum of boson stars, showing that it is remarkably different from the QNM spectrum of BHs and lending support to the feasibility of no-hair tests using QNM measurements [29][30][31].…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Introductionsupporting

confidence: 82%

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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“…4c of Ref. [22] shows that many modes are indeed present in the signal, that the l = 2 component dominates the energy emission, and that all modes with n < 12 are necessary to fit the waveform (modes with n = 5 − 10 being dominant).…”

Section: Exotic Strawmen: Boson Star Hair Countingmentioning

confidence: 96%

Supermassive Black Holes or Boson Stars? Hair Counting With Gravitational Wave Detectors

Berti¹,

Cardoso

2006

Int. J. Mod. Phys. D

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The evidence for supermassive Kerr black holes in galactic centers is strong and growing, but only the detection of gravitational waves will convincingly rule out other possibilities to explain the observations. The Kerr spacetime is completely specified by the first two multipole moments: mass and angular momentum. This is usually referred to as the "no-hair theorem", but it is really a "two-hair" theorem. If general relativity is the correct theory of gravity, the most plausible alternative to a supermassive Kerr black hole is a rotating boson star. Numerical calculations indicate that the spacetime of rotating boson stars is determined by the first three multipole moments ("threehair theorem"). The Laser Interferometer Space Antenna (LISA) could accurately measure the oscillation frequencies of these supermassive objects. We propose to use these measurements to "count their hair", unambiguously determining their nature and properties.

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“…For example, there are models of dark matter which use EKG in the weak field limit [50][51][52][53]. One example of relativistic scalar field is boson stars [54][55][56][57][58]. Therefore, it is interesting to ask if gravitational wave detection can be used to distinguish BBH collisions in f (R) theory from another system which also contains scalar fields.…”

Section: Dynamics Of the Binary Black Hole Induced By The Scalar Fieldmentioning

confidence: 99%

Binary black hole mergers inf(R)theory

2013

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In the near future, gravitational wave detection is set to become an important observational tool for astrophysics. It will provide us with an excellent means to distinguish different gravitational theories. In effective form, many gravitational theories can be cast into an f (R) theory. In this article, we study the dynamics and gravitational waveform of an equal-mass binary black hole system in f (R) theory. We reduce the equations of motion in f (R) theory to the Einstein-Klein-Gordon coupled equations. In this form, it is straightforward to modify our existing numerical relativistic codes to simulate binary black hole mergers in f (R) theory. We considered binary black holes surrounded by a shell of scalar field. We solve the initial data numerically using the Olliptic code. The evolution part is calculated using the extended AMSS-NCKU code. Both codes were updated and tested to solve the problem of binary black holes in f (R) theory. Our results show that the binary black hole dynamics in f (R) theory is more complex than in general relativity. In particular, the trajectory and merger time are strongly affected. Via the gravitational wave, it is possible to constrain the quadratic part parameter of f (R) theory in the range |a2| < 10 11 m 2 . In principle, a gravitational wave detector can distinguish between a merger of binary black hole in f (R) theory and the respective merger in general relativity. Moreover, it is possible to use gravitational wave detection to distinguish between f (R) theory and a non self-interacting scalar field model in general relativity.

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Evolution of 3D boson stars with waveform extraction

Cited by 45 publications

References 54 publications

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

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

Supermassive Black Holes or Boson Stars? Hair Counting With Gravitational Wave Detectors

Binary black hole mergers inf(R)theory

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