Off-axis Prompt X-Ray Transients from the Cocoon of Short Gamma-Ray Bursts

Lazzati, Davide; López-Cámara, Diego; Cantiello, Matteo; Morsony, Brian J.; Perna, Rosalba; Workman, Jared C.

doi:10.3847/2041-8213/aa8f3d

Cited by 149 publications

(174 citation statements)

References 70 publications

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“…• [1], this observation suggests a detection of an off-axis gamma-ray burst emission or cocoon emission arising from an ultra-relativistic jet launched at the merger [28,29]. However, the production of such an ultra-relativistic jet in numerical-relativity simulations is beyond the scope of our paper.…”

Section: Introductionmentioning

confidence: 91%

Modeling GW170817 based on numerical relativity and its implications

et al. 2017

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Gravitational-wave observation together with a large number of electromagnetic observations shows that the source of the latest gravitational-wave event, GW170817, detected primarily by advanced LIGO, is the merger of a binary neutron star. We attempt to interpret this observational event based on our results of numerical-relativity simulations performed so far paying particular attention to the optical and infra-red observations. We finally reach a conclusion that this event is described consistently by the presence of a long-lived hypermassive or supramassive neutron star as the merger remnant, because (i) significant contamination by lanthanide elements along our line of sight to this source can be avoided by the strong neutrino irradiation from it and (ii) it could play a crucial role to produce an ejecta component of appreciable mass with fast motion in the postmerger phase. We also point out that (I) the neutron-star equation of state has to be sufficiently stiff (i.e., the maximum mass of cold spherical neutron stars, Mmax, has to be appreciably higher than 2M ) in order that a long-lived massive neutron star can be formed as the merger remnant for the binary systems of GW170817, for which the initial total mass is 2.73M and (II) no detection of relativistic optical counterpart suggests a not-extremely high value of Mmax approximately as 2.15-2.25M .

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Section: Introductionmentioning

confidence: 91%

Modeling GW170817 based on numerical relativity and its implications

et al. 2017

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“…In others studies, the adopted index differs (e.g. n = 2 in Gottlieb et al 2018b;Xie et al 2018;Lazzati et al 2017). For the velocity profile, the adopted maximum velocity vej in different studies varies.…”

Section: Numerical Relativity Simulations and The Dynamical Ejectamentioning

confidence: 99%

Jet Propagation in Neutron Star Mergers and GW170817

Hamidani

Kiuchi

Ioka

2019

Monthly Notices of the Royal Astronomical Society

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The gravitational wave event from the binary neutron star (BNS) merger GW170817 and the following multi-messenger observations present strong evidence for i) merger ejecta expanding with substantial velocities and ii) a relativistic jet which had to propagate through the merger ejecta. The ejecta's expansion velocity is not negligible for the jet head motion, which is a fundamental difference from the other systems like collapsars and active galactic nuclei. Here we present an analytic model of the jet propagation in an expanding medium. In particular, we notice a new term in the expression of the breakout time and velocity. In parallel, we perform a series of over a hundred 2D numerical simulations of jet propagation. The BNS merger ejecta is prepared based on numerical relativity simulations of a BNS merger with the highestresolution to date. We show that our analytic results agree with numerical simulations over a wide parameter space. Then we apply our analytic model to GW170817, and obtain two solid constraints on: i) the central engine luminosity as L iso,0 ∼ 3 × 10 49 − 2.5 × 10 52 erg s −1 , and on ii) the delay time between the merger and engine activation t 0 − t m < 1.3 s. The engine power implies that the apparently-faint short gamma-ray burst (sGRB) sGRB 170817A is similar to typical sGRBs if observed on-axis.

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“…Comparison between the jet structure predicted by our model and the results of numerical simulations byLazzati et al (2017). The upper panel refers to the distribution of kinetic energy per unit solid angle, while the lower panel shows the average Lorentz factor diminished by one.…”

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confidence: 93%

Gamma-ray burst jet propagation, development of angular structure, and the luminosity function

Salafia

Barbieri

Ascenzi

et al. 2020

A&A

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The fate and observable properties of gamma-ray burst jets depend crucially on their interaction with the progenitor material that surrounds the central engine. We present a semi-analytical model of such interaction, which builds upon several previous analytical and numerical works, aimed at predicting the angular distribution of jet and cocoon energy and Lorentz factor after breakout, given the properties of the ambient material and of the jet at launch. Using this model, we construct synthetic populations of structured jets, assuming either a collapsar (for long gamma-ray bursts -LGRBs) or a binary neutron star merger (for short gamma-ray bursts -SGRBs) as progenitor. We assume all progenitors to be identical, and we allow little variability in the jet properties at launch: our populations therefore feature a quasi-universal structure. These populations are able to reproduce the main features of the observed LGRB and SGRB luminosity functions, although several uncertainties and caveats remain to be addressed.

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Off-axis Prompt X-Ray Transients from the Cocoon of Short Gamma-Ray Bursts

Cited by 149 publications

References 70 publications

Modeling GW170817 based on numerical relativity and its implications

Modeling GW170817 based on numerical relativity and its implications

Jet Propagation in Neutron Star Mergers and GW170817

Gamma-ray burst jet propagation, development of angular structure, and the luminosity function

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