Gravitational Radiation from Gamma‐Ray Burst Progenitors

Kobayashi, S.; Mészáros, P.

doi:10.1086/374733

Cited by 127 publications

(166 citation statements)

References 42 publications

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“…For an initially static star v (0) = 0. 7 In a general analysis one could pick ε = α and use the full expression for a ext i in Eq. (3.2).…”

Section: B Second Order Eulerian Perturbation Theorymentioning

confidence: 99%

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Are neutron stars crushed? Gravitomagnetic tidal fields as a mechanism for binary-induced collapse

Favata

2006

Phys. Rev. D

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Numerical simulations of binary neutron stars by Wilson, Mathews, and Marronetti indicated that neutron stars that are stable in isolation can be made to collapse to black holes when placed in a binary. This claim was surprising as it ran counter to the Newtonian expectation that a neutron star in a binary should be more stable, not less. After correcting an error found by Flanagan, Wilson and Mathews found that the compression of the neutron stars was significantly reduced but not eliminated. This has motivated us to ask the following general question: Under what circumstances can general relativistic tidal interactions cause an otherwise stable neutron star to be compressed? We have found that if a non-rotating neutron star possesses a current quadrupole moment, interactions with a gravitomagnetic tidal field can lead to a compressive force on the star. If this current quadrupole is induced by the gravitomagnetic tidal field, it is related to the tidal field by an equation-of-state-dependent constant called the gravitomagnetic Love number. This is analogous to the Newtonian Love number that relates the strength of a Newtonian tidal field to the induced mass quadrupole moment of a star. The compressive force is almost never larger than the Newtonian tidal interaction that stabilizes the neutron star against collapse. In the case in which a current quadrupole is already present in the star (perhaps as an artifact of a numerical simulation), the compressive force can exceed the stabilizing one, leading to a net increase in the central density of the star. This increase is small ( 1%) but could, in principle, cause gravitational collapse in a star that is close to its maximum mass. This paper also reviews the history of the Wilson-MathewsMarronetti controversy and, in an appendix, extends the discussion of tidally-induced changes in the central density to rotating stars.

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“…For an initially static star v (0) = 0. 7 In a general analysis one could pick ε = α and use the full expression for a ext i in Eq. (3.2).…”

Section: B Second Order Eulerian Perturbation Theorymentioning

confidence: 99%

“…7-15 of [5]). The detection of GWs from NS/NS coalescences could yield information about the equation of state (EOS) of ultra-dense nuclear matter, and about short-duration gamma-ray bursts [6,7]. Accurate predictions of the GW signal will be important for these purposes.…”

Section: Introductionmentioning

confidence: 99%

Are neutron stars crushed? Gravitomagnetic tidal fields as a mechanism for binary-induced collapse

Favata

2006

Phys. Rev. D

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“…Fragmentation instabilities could be produced in the core or in the disc (Fryer et al, 2002;Kobayashi & Mészáros, 2003). Rapid rotation could also give rise to rotational instabilities in the protoneutron star remnant (Dimmelmeier et al, 2008;Corsi & Mészáros, 2009b;Piro & Ott, 2011;Piro & Thrane, 2012) A number of studies have suggested there exists a sub-population of LGRBs known as low-luminosity GRBs (ll GRBs).…”

Section: Long Gamma Ray Bursts As Multi-messenger Targets For Gwsmentioning

confidence: 99%

Hunting Gravitational Waves with Multi-Messenger Counterparts: Australia’s Role

Howell

Rowlinson

Coward

et al. 2015

Publ. Astron. Soc. Aust.

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The first observations by a worldwide network of advanced interferometric gravitational wave detectors offer a unique opportunity for the astronomical community. At design sensitivity, these facilities will be able to detect coalescing binary neutron stars to distances approaching 400 Mpc, and neutron star-black hole systems to 1 Gpc. Both of these sources are associated with gamma ray bursts which are known to emit across the entire electromagnetic spectrum. Gravitational wave detections provide the opportunity for "multi-messenger" observations, combining gravitational wave with electromagnetic, cosmic ray or neutrino observations. This review provides an overview of how Australian astronomical facilities and collaborations with the gravitational wave community can contribute to this new era of discovery, via contemporaneous follow-up observations from the radio to the optical and high energy. We discuss some of the frontier discoveries that will be made possible when this new window to the Universe is opened.

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“…A large variety of possible GW emitting mechanisms within these systems have been proposed, with some models predicting GW spectra that would be observable from distances of a few Mpc with initial LIGO and Virgo (Fryer et al 2002;Kobayashi & Mészáros 2003a;Corsi & Mészáros 2009;Piro & Pfahl 2007;Korobkin et al 2011;Kiuchi et al 2011). The afterglows of LGRBs, like the afterglows of SGRBs, typically show power law fading with α = 1−1.5.…”

Section: Stellar Core Collapsementioning

confidence: 99%

Implementation and testing of the first prompt search for gravitational wave transients with electromagnetic counterparts

Abadie

Abbott

et al. 2012

A&A

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Article published by EDP Sciences A124, page 1 of 15 A&A 539, A124 (2012) ABSTRACT Aims. A transient astrophysical event observed in both gravitational wave (GW) and electromagnetic (EM) channels would yield rich scientific rewards. A first program initiating EM follow-ups to possible transient GW events has been developed and exercised by the LIGO and Virgo community in association with several partners. In this paper, we describe and evaluate the methods used to promptly identify and localize GW event candidates and to request images of targeted sky locations. Methods. During two observing periods (Dec. 17, 2009 to Jan. 8, 2010 and Sep. 2 to Oct. 20, 2010, a low-latency analysis pipeline was used to identify GW event candidates and to reconstruct maps of possible sky locations. A catalog of nearby galaxies and Milky Way globular clusters was used to select the most promising sky positions to be imaged, and this directional information was delivered to EM observatories with time lags of about thirty minutes. A Monte Carlo simulation has been used to evaluate the low-latency GW pipeline's ability to reconstruct source positions correctly.Results. For signals near the detection threshold, our low-latency algorithms often localized simulated GW burst signals to tens of square degrees, while neutron star/neutron star inspirals and neutron star/black hole inspirals were localized to a few hundred square degrees. Localization precision improves for moderately stronger signals. The correct sky location of signals well above threshold and originating from nearby galaxies may be observed with ∼50% or better probability with a few pointings of wide-field telescopes.

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Gravitational Radiation from Gamma‐Ray Burst Progenitors

Cited by 127 publications

References 42 publications

Are neutron stars crushed? Gravitomagnetic tidal fields as a mechanism for binary-induced collapse

Are neutron stars crushed? Gravitomagnetic tidal fields as a mechanism for binary-induced collapse

Hunting Gravitational Waves with Multi-Messenger Counterparts: Australia’s Role

Implementation and testing of the first prompt search for gravitational wave transients with electromagnetic counterparts

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