scholarly journals The Rate of Short-Duration Gamma-Ray Bursts in the Local Universe

Galaxies ◽  
2018 ◽  
Vol 6 (4) ◽  
pp. 130 ◽  
Author(s):  
Soheb Mandhai ◽  
Nial Tanvir ◽  
Gavin Lamb ◽  
Andrew Levan ◽  
David Tsang
Keyword(s):  
Neutron Star ◽  
Short Duration ◽  
Gamma Ray ◽  
Local Population ◽  
Gamma Ray Burst ◽  
Binary Neutron Star ◽  
Upper Limit ◽  
Transient Source ◽  
The Galaxy ◽  
Short Grbs

Following the faint gamma-ray burst, GRB 170817A, coincident with a gravitational wave-detected binary neutron star merger at d ∼ 40 Mpc, we consider the constraints on a local population of faint short duration GRBs (defined here broadly as T 90 < 4 s). We review proposed low-redshift short-GRBs and consider statistical limits on a d ≲ 200 Mpc population using Swift/Burst Alert Telescope (BAT), Fermi/Gamma-ray Burst Monitor (GBM), and Compton Gamma-Ray Observatory (CGRO) Burst and Transient Source Experiment (BATSE) GRBs. Swift/BAT short-GRBs give an upper limit for the all-sky rate of < 4 y − 1 at d < 200 Mpc, corresponding to < 5% of SGRBs. Cross-correlation of selected CGRO/BATSE and Fermi/GBM GRBs with d < 100 Mpc galaxy positions returns a weaker constraint of ≲ 12 y − 1 . A separate search for correlations due to SGR giant flares in nearby ( d < 11 Mpc) galaxies finds an upper limit of < 3 y − 1 . Our analysis suggests that GRB 170817A-like events are likely to be rare in existing SGRB catalogues. The best candidate for an analogue remains GRB 050906, where the Swift/BAT location was consistent with the galaxy IC 0327 at d ≈ 132 Mpc. If binary neutron star merger rates are at the high end of current estimates, then our results imply that at most a few percent will be accompanied by detectable gamma-ray flashes in the forthcoming LIGO/Virgo science runs.

scholarly journals Binary Neutron Star (BNS) Merger: What We Learned from Relativistic Ejecta of GW/GRB 170817A

Physics ◽  
2019 ◽  
Vol 1 (2) ◽  
pp. 194-228 ◽  
Author(s):  
Houri Ziaeepour
Keyword(s):  
Neutron Star ◽  
Gravitational Waves ◽  
Gamma Ray ◽  
Lorentz Factor ◽  
Prompt Gamma ◽  
External Shocks ◽  
Binary Neutron Star ◽  
Tidal Forces ◽  
Relativistic Jet ◽  
Short Grbs

Gravitational Waves (GW) from coalescence of a Binary Neutron Star (BNS) and its accompanying short Gamma-Ray Burst (GRB) GW/GRB 170817A confirmed the presumed origin of these puzzling transients and opened up the way for relating properties of short GRBs to those of their progenitor stars and their surroundings. Here we review an extensive analysis of the prompt gamma-ray and late afterglows of this event. We show that a fraction of polar ejecta from the merger had been accelerated to ultra-relativistic speeds. This structured jet had an initial Lorentz factor of about 260 in our direction, which was O ( 10 ∘ ) from the jet’s axis, and was a few orders of magnitude less dense than in typical short GRBs. At the time of arrival to circum-burst material the ultra-relativistic jet had a close to Gaussian profile and a Lorentz factor ≳ 130 in its core. It had retained in some extent its internal collimation and coherence, but had extended laterally to create mildly relativistic lobes—a cocoon. Its external shocks on the far from center inhomogeneous circum-burst material and low density of colliding shells generated slowly rising afterglows, which peaked more than 100 days after the prompt gamma-ray. The circum-burst material was somehow correlated with the merger. As non-relativistic outflows or tidally ejected material during BNS merger could not have been arrived to the location of the external shocks before the relativistic jet, circum-burst material might have contained recently ejected materials from resumption of internal activities, faulting and mass loss due to deformation and breaking of stars crusts by tidal forces during latest stages of their inspiral but well before their merger. By comparing these findings with the results of relativistic Magneto-Hydro-Dynamics (MHD) simulations and observed gravitational waves we conclude that progenitor neutron stars were most probably old, had close masses and highly reduced magnetic fields.

scholarly journals NECESSARY CONDITIONS FOR SHORT GAMMA-RAY BURST PRODUCTION IN BINARY NEUTRON STAR MERGERS

2014 ◽  
Vol 788 (1) ◽  
pp. L8 ◽  
Author(s):  
Ariadna Murguia-Berthier ◽  
Gabriela Montes ◽  
Enrico Ramirez-Ruiz ◽  
Fabio De Colle ◽  
William H. Lee
Keyword(s):  
Neutron Star ◽  
Gamma Ray ◽  
Necessary Conditions ◽  
Gamma Ray Burst ◽  
Binary Neutron Star

scholarly journals Protomagnetar research through an analysis of the X-ray plateau in the multi-messengar era

2020 ◽  
Vol 641 ◽  
pp. A56
Author(s):  
Xiaoxiao Ren ◽  
Daming Wei ◽  
Zhenyu Zhu ◽  
Yan Yan ◽  
Chengming Li
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Gravitational Wave ◽  
Gamma Ray ◽  
Equations Of State ◽  
Electromagnetic Emission ◽  
Gamma Ray Bursts ◽  
Gamma Ray Burst ◽  
X Ray ◽  
Binary Neutron Star

The joint detection of the gravitational wave signal and the electromagnetic emission from a binary neutron star merger can place unprecedented constraint on the equation of state of supranuclear matter. Although a variety of electromagnetic counterparts have been observed for GW170817, including a short gamma-ray burst, kilonova, and the afterglow emission, the nature of the merger remnant is still unclear, however. The X-ray plateau is another important characteristics of short gamma-ray bursts. This plateau is probably due to the energy injection from a rapidly rotating magnetar. We investigate what we can learn from the detection of a gravitational wave along with the X-ray plateau. In principle, we can estimate the mass of the merger remnant if the X-ray plateau is caused by the central magnetar. We selected eight equations of state that all satisfy the constraint given by the gravitational wave observation, and then calculated the mass of the merger remnants of four short gamma-ray bursts with a well-measured X-ray plateau. If, on the other hand, the mass of the merger remnant can be obtained by gravitational wave information, then by comparing the masses derived by these two different methods can further constrain the equation of state. We discuss the possibility that the merger product is a quark star. In addition, we estimate the possible mass range for the recently discovered X-ray transient CDF-S XT2 that probably originated from a binary neutron star merger. Finally, under the assumption that the post-merger remnant of GW170817 was a supramassive neutron star, we estimated the allowed parameter space of the supramassive neutron star and find that in this case, the magnetic dipole radiation energy is so high that it may have some effects on the short gamma-ray burst and kilonova emission. The lack of detection of these effects suggests that the merger product of GW170817 may not be a supermassive neutron star.

scholarly journals Binary Neutron Star and Short Gamma-Ray Burst Simulations in Light of GW170817

Galaxies ◽  
2018 ◽  
Vol 6 (4) ◽  
pp. 119 ◽  
Author(s):  
Antonios Nathanail
Keyword(s):  
Neutron Star ◽  
Gravitational Wave ◽  
Electromagnetic Radiation ◽  
Numerical Simulations ◽  
Gravitational Waves ◽  
Gamma Ray ◽  
Numerical Relativity ◽  
Gamma Ray Burst ◽  
Binary Neutron Star ◽  
The Status

In the dawn of the multi-messenger era of gravitational wave astronomy, which was marked by the first ever coincident detection of gravitational waves and electromagnetic radiation, it is important to take a step back and consider our current established knowledge. Numerical simulations of binary neutron star mergers and simulations of short GRB jets must combine efforts to understand such complicated and phenomenologically rich explosions. We review the status of numerical relativity simulations with respect to any jet or magnetized outflow produced after merger. We compare what is known from such simulations with what is used and obtained from short GRB jet simulations propagating through the BNS ejecta. We then review the established facts on this topic, as well as discuss things that need to be revised and further clarified.

scholarly journals The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. VIII. A Comparison to Cosmological Short-duration Gamma-Ray Bursts

2017 ◽  
Vol 848 (2) ◽  
pp. L23 ◽  
Author(s):  
W. Fong ◽  
E. Berger ◽  
P. K. Blanchard ◽  
R. Margutti ◽  
P. S. Cowperthwaite ◽  
...  
Keyword(s):  
Neutron Star ◽  
Short Duration ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Binary Neutron Star

scholarly journals A Genuinely Short Gamma-Ray Burst from Massive Star Core Collapse

2020 ◽  
Author(s):  
Binbin Zhang ◽  
Zi-Ke Liu ◽  
Zong-Kai Peng ◽  
Ye Li ◽  
H.-J. Lu ◽  
...  
Keyword(s):  
Neutron Star ◽  
Massive Star ◽  
Gamma Ray ◽  
Sensitivity Threshold ◽  
Core Collapse ◽  
Binary Neutron Star ◽  
Long Duration ◽  
Multi Wavelength ◽  
Short Grbs ◽  
Bright Emission

Abstract Gamma-ray bursts have been phenomenologically classified into long and short populations based on whether the observed duration is longer or shorter than two seconds. Multi-wavelength and multi-messenger observations in recent years have revealed that in general long GRBs originate from massive star core collapse events, whereas short GRBs originate from binary neutron star mergers. It has been known that the duration criterion is sometimes unreliable, and multi-wavelength criteria are needed to identify the physical origin of a particular GRB. Some apparently long GRBs have been suggested to have a neutron star merger origin, whereas some apparently short GRBs have been attributed to genuinely long GRBs whose short, bright emission is above the detector's sensitivity threshold. Still, there has been no known case that a GRB is genuinely short but originates from death of a massive star. Here we report the comprehensive analysis of the multi-wavelength data of a bright short GRB 200826A. This burst has a sharp 1-second spike, which is not part of an underlying long-duration event. Its other observational properties are, however, inconsistent with those of other short GRBs believed to originate from binary neutron star mergers. Rather, these properties resemble those of long GRBs. This burst presents a challenge to the traditional GRB classification scheme and reveals a class of core-collapse-origin GRBs with genuinly short durations.

scholarly journals ALMA and GMRT Constraints on the Off-axis Gamma-Ray Burst 170817A from the Binary Neutron Star Merger GW170817

2017 ◽  
Vol 850 (2) ◽  
pp. L21 ◽  
Author(s):  
S. Kim ◽  
S. Schulze ◽  
L. Resmi ◽  
J. González-López ◽  
A. B. Higgins ◽  
...  
Keyword(s):  
Neutron Star ◽  
Gamma Ray ◽  
Gamma Ray Burst ◽  
Binary Neutron Star

scholarly journals The Swift short gamma-ray burst rate density: implications for binary neutron star merger rates

2012 ◽  
Vol 425 (4) ◽  
pp. 2668-2673 ◽  
Author(s):  
D. M. Coward ◽  
E. J. Howell ◽  
T. Piran ◽  
G. Stratta ◽  
M. Branchesi ◽  
...  
Keyword(s):  
Neutron Star ◽  
Gamma Ray ◽  
Gamma Ray Burst ◽  
Binary Neutron Star

scholarly journals Ready, Set, Launch: Time Interval between a Binary Neutron Star Merger and Short Gamma-Ray Burst Jet Formation

2020 ◽  
Vol 895 (2) ◽  
pp. L33 ◽  
Author(s):  
Paz Beniamini ◽  
Rodolfo Barniol Duran ◽  
Maria Petropoulou ◽  
Dimitrios Giannios
Keyword(s):  
Neutron Star ◽  
Gamma Ray ◽  
Time Interval ◽  
Jet Formation ◽  
Gamma Ray Burst ◽  
Binary Neutron Star

scholarly journals Are short GRBs powered by magnetars?

2011 ◽  
Vol 7 (S279) ◽  
pp. 297-300 ◽  
Author(s):  
Paul T. O'Brien ◽  
Antonia Rowlinson
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Binary System ◽  
Short Duration ◽  
Gamma Ray ◽  
Large Fraction ◽  
Light Curves ◽  
The Standard Model ◽  
Star Binary ◽  
Short Grbs

AbstractThe 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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