The Massive Pulsar PSR J1614–2230: Linking Quantum Chromodynamics, Gamma-Ray Bursts, and Gravitational Wave Astronomy

Özel, Feryal; Psaltis, Dimitrios; Ransom, S. M.; Demorest, Paul; Alford, Mark

doi:10.1088/2041-8205/724/2/l199

Cited by 165 publications

(126 citation statements)

References 25 publications

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“…When assuming that most type-I GRBs are created by NS-BH mergers, an opening angle of smaller than ∼1 • is excluded. This plot also indicates that η might not be too small, agreeing with the results obtained in Belczynski et al (2008b) and Ozel et al (2010).…”

Section: Constraints On Grb Parameterssupporting

confidence: 90%

“…Even then, it is hard to estimate the fraction of mergers that might create a type-I GRB; a recent investigation inferred η = 0.01−0.4 in the case of NS-BH systems , with an even larger spread in the case of NS-NS systems ). The recent discovery of a 2 M neutron star (Demorest et al 2010b) makes it far more plausible that two coalescing neutron stars generate type-I GRBs (Ozel et al 2010), resulting in a much larger value of η. A value of η = 0.5 is used as a first guess for the latter analysis, but we investigate also the outcome of choosing any possible value between 0 and 1.…”

Section: Fraction Of Mergers Producing a Type-i Grbmentioning

confidence: 99%

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Estimation of compact binary coalescense rates from short gamma-ray burst redshift measurements

Dietz

2011

A&A

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Aims. We aim to estimate the rate of compact binaries and compare these with similar estimates based on either the observation of these binaries or population synthesis models. Since the merger of these compact objects are likely to produce short gamma-ray bursts, conclusions about the opening angle of these bursts can be made. Methods. We use a set of observed redshift measurements of short gamma-ray bursts to model the rate of these merger events in the nearby universe. Various corrections are included in the calculation, such as the field-of-view of the satellite missions, the beaming factors of gamma-ray burst and other parameters. Results. The computed rate estimates are compared to other rate estimates, based on observations of binary neutron stars and population synthesis models. Given the upper limit established by LIGO/Virgo measurements, it is possible to draw conclusions about the beaming angle of gamma-ray bursts.

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Section: Constraints On Grb Parameterssupporting

confidence: 90%

Section: Fraction Of Mergers Producing a Type-i Grbmentioning

confidence: 99%

Estimation of compact binary coalescense rates from short gamma-ray burst redshift measurements

Dietz

2011

A&A

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“…Ozel [18] and Lattimer [19] gave first studies on the implications of the new mass limits from PSR J1614-2230 for quark and hybrid stars in the quark bag model. Recently, Bonanno & Sedrakian [20] has succeeded in obtaining massive HS.…”

Section: Introductionmentioning

confidence: 99%

Maximum mass of a hybrid star having a mixed-phase region based on constraints set by the pulsar PSR J1614-2230

Mallick

2013

Phys. Rev. C

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Recent observation of pulsar PSR J1614-2230 with mass about 2 solar masses poses a severe constraint on the equations of state (EOS) of matter describing stars under extreme conditions. Neutron stars (NS) can reach the mass limits set by PSR J1614-2230. But stars having hyperons or quark stars (QS) having boson condensates, with softer EOS can barely reach such limits and are ruled out. QS with pure strange matter also cannot have such high mass unless the effect of strong coupling constant or color superconductivity are considered. In this work I try to calculate the upper mass limit for a hybrid stars (HS) having a quark-hadron mixed phase. The hadronic matter (having hyperons) EOS is described by relativistic mean field theory and for the quark phase I use the simple MIT bag model. I construct the intermediate mixed phase using Glendenning construction. HS with a mixed phase cannot reach the mass limit set by PSR J1614-2230 unless I assume a density dependent bag constant. For such case the mixed phase region is small. The maximum mass of a mixed hybrid star obtained with such mixed phase region is 2.01M ⊙ .

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“…The model used here is as described in Zhang & Mészáros (2001) and used by Troja et al (2007), Lyons et al (2010), Rowlinson et al (2010). This model is consistent with the late-time residual spin-down phase driving a relativistic magnetar wind as described in Metzger et al (2011).…”

Section: Magnetar Model Fitsmentioning

confidence: 55%

“…Morrison, Baumgarte, & Shapiro (2004) showed that the rotation of the NS could increase the maximum mass by ∼ 50% and hence NS mergers could often result in a NS. Ozel et al (2010) further showed that in such a merger the collapse to a BH can be delayed or not occur at all. Thus, it seems reasonable to assume that many NS binary mergers could result in a magnetar in a SGRB.…”

Section: P T O'brien and A Rowlinsonmentioning

confidence: 98%

Are short GRBs powered by magnetars?

O’Brien¹,

Rowlinson

2011

Proc. IAU

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Abstract. The standard model for a short duration Gamma-Ray Burst (GRB) involves the merger of a neutron star binary system, resulting in a black hole which accretes for a brief period of time. However, some of the short-duration GRBs observed by the Swift satellite show features in their light curves which are difficult to explain in this model. As an alternative, we examine the light curves of the Swift short GRB sample to see if they can be explained by the presence of a highly magnetised, rapidly rotating pulsar, or magnetar. We find that magnetars may be present in a large fraction of short bursts, and discuss briefly how this model can be tested using the next generation of gravity-wave observatories.

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The Massive Pulsar PSR J1614–2230: Linking Quantum Chromodynamics, Gamma-Ray Bursts, and Gravitational Wave Astronomy

Cited by 165 publications

References 25 publications

Estimation of compact binary coalescense rates from short gamma-ray burst redshift measurements

Estimation of compact binary coalescense rates from short gamma-ray burst redshift measurements

Maximum mass of a hybrid star having a mixed-phase region based on constraints set by the pulsar PSR J1614-2230

Are short GRBs powered by magnetars?

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