Short-hard gamma-ray bursts

By E. Nakar. 2007

750 citations recorded by the source corpus.

Two types of gamma-ray bursts (GRBs) are observed: short-duration hard spectrum GRBs and long-duration soft spectrum GRBs. For many years long GRBs were the focus of intense research while the lack of observational data limited the study of short-hard GRBs (SHBs). In 2005 a breakthrough occurred following the first detections of SHB afterglows, longer wavelength emission that follows the burst of gamma-rays. Similarly to long GRBs, afterglow detections led to the identification of SHB host galaxies and measurement of their redshifts. These observations established that SHBs are cosmological relativistic sources that, unlike long GRBs, do not originate from the collapse of massive stars, and therefore constitute a distinct physical phenomenon. One viable model for SHB origin is the coalescence of compact binary systems (double neutron stars or a neutron star and a black hole), in which case SHBs are the electromagnetic counterparts of strong gravitational-wave sources. The theoretical and observational study of SHBs following the recent pivotal discoveries is reviewed, along with new theoretical results that are presented here for the first time.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/a8f1df266a09dfa346b90bc9bb1e2887b2023451

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In Astronomy and Astrophysics

1. Bing Zhang
2. B. Metzger
3. E. Berger
4. E. Quataert
5. D. Kasen
6. E. Nakar
7. Pawan Kumar
8. Stephan Rosswog

In Instrumentation

1. Bing Zhang
2. P. Hopkins
3. L. Hernquist
4. Risa Wechsler
5. B. Metzger
6. C. Conroy
7. Simon D. M. White
8. E. Berger

Citations in the corpus

• Comprehensive nucleosynthesis analysis for ejecta of compact binary mergers (2014, background): “Strong arguments suggest that their remnants are good candidates for the still enigmatic central engines of short gamma-ray bursts (GRBs; see, e.g. Nakar 2007; Berger 2014 for reviews).”
• Short-Duration Gamma-Ray Bursts (2013, background): “…first few short GRB host galaxies from 2005, led several groups to conclude that early-type galaxies dominate the sample at a ratio of about 2:1, and that the progenitors are therefore exceedingly old, with a characterstic age of∼ 5− 10 Gyr (Prochaska et al. 2006, Nakar 2007, Gal-Yam et al. 2008).”
• THE AFTERGLOWS OF SWIFT-ERA GAMMA-RAY BURSTS. II. TYPE I GRB VERSUS TYPE II GRB OPTICAL AFTERGLOWS (2008, background): “In some cases, an even lower density n (to be consistent with the intergalactic medium outside the host galaxy - as expected to happen for some short GRBs with large kick velocities) is needed to account for the faintness of the afterglows (Nakar 2007).”
• ELECTROMAGNETIC TRANSIENTS POWERED BY NUCLEAR DECAY IN THE TIDAL TAILS OF COALESCING COMPACT BINARIES (2011, background): “Merging compact binaries are the primary candidate for direct detection of gravitational waves (GWs) by LIGO (Abbott et al. 2008), and are thought to be the progenitors of short gamma-ray bursts (SGRBs)(c.f. Lee & Ramirez-Ruiz 2007; Rosswog 2007; Nakar 2007; Gehrels et al. 2009).”
• The long-term evolution of neutron star merger remnants – I. The impact of r-process nucleosynthesis (2013, background): “The importance of compact binary mergers as sources of gravitational waves (GW; e.g. Cutler & Flanagan 1994; Maggiore 2007) and as central engines of short Gamma-ray bursts (Eichler et al. 1989; Narayan et al. 1991; Piran 2004; Nakar 2007; Lee & Ramirez-Ruiz 2007) has been appreciated for decades.”
• Neutrino-driven winds from neutron star merger remnants (2014, background): “…of the properties expected from compact binary mergers with those observed in sGRBs is not completely free of tension (see Piran 2004; Lee & Ramirez-Ruiz 2007; Nakar 2007; Gehrels, E-mail: albino.perego@physik.tu-darmstadt.de Ramirez-Ruiz & Fox 2009; Berger 2011, 2013, for recent reviews).”
• THE LARGE AREA TELESCOPE ON THE FERMI GAMMA-RAY SPACE TELESCOPE MISSION (2009, background): “Short-duration bursts are often located in much lower star-formation rate regions of the host galaxy, suggesting that in some cases these bursts arise from the coalescence of compact objects (Bloom et al. 2006; Nakar 2007).”
• Compact binary coalescences in the band of ground-based gravitational-wave detectors (2009, background): “However, extrapolating from the rate of observed SGRBs, as attempted, for example, in [27], is highly uncertain, because of unknown selection effects such as SGRB beaming fractions [55], which may be different for field and cluster SGRBs [34]; additionally, binary mergers involving NSs are not the o”
• THE OBSERVABLE SIGNATURES OF GRB COCOONS (2016, background): “The uncertainty concerning typical SGRB parameters is much larger than the uncertainty concerning LGRBs (see Nakar 2007; Berger 2014, for a review)).”
• The electromagnetic signals of compact binary mergers (2012, background): “Therefore, assuming that short GRBs are beamed, the detection of the common ∼1049 erg bursts in a blind survey, even with next generation radio facilities, is unlikely (Nakar 2007).”
• The cocoon emission - an electromagnetic counterpart to gravitational waves from neutron star mergers (2017, background): “However, these bursts are beamed and in most cases we won’t observe the accompanying GRB (see Nakar 2007 for a review).”
• Time-dependent models of accretion discs formed from compact object mergers (2008, background): “Thus, even assuming a modest radiative efficiency for the outflow of ǫw ∼ 0.1, the Lorentz factor Γ of a neutrino-heated disk wind must obey Γ ≃ Lγ/[ǫwṀν(r∗)c 2] ∼ 5, which is inconsistent with existing compactness constraints on short GRBs (Nakar 2007).”
• NEUTRINO SIGNATURES AND THE NEUTRINO-DRIVEN WIND IN BINARY NEUTRON STAR MERGERS (2008, background): “Moreover, such baryonic pollution along the polar direction may affect any subsequent relativistic ejecta, although the wind fromthe SMNS may last for only a short time, perhaps 100 ms. Travelling at a tenth the speed of light, it will reach only out to 0.01 light-second, thus much shorter than the ”
• Mass Ejection from the Remnant of a Binary Neutron Star Merger: Viscous-radiation Hydrodynamics Study (2017, background): “The remnants of binary neutron star mergers have been considered to power relativistic jets that would drive shortduration gamma-ray bursts (Eichler et al. 1989; Nakar 2007).”
• INTEGRAL Detection of the First Prompt Gamma-Ray Signal Coincident with the Gravitational-wave Event GW170817 (2017, background): “…(GRBs) with a duration below about 2 s, known as short gamma-ray bursts (sGRBs), are the product of a binary neutron star (BNS) merger and that gamma-rays are produced in the collimated ejecta following the coalescence (e.g., Blinnikov et al. 1984; Nakar 2007; Gehrels & Meszaros 2012; Berger 2014).”
• The birth of black holes: neutron star collapse times, gamma-ray bursts and fast radio bursts (2014, background): “…M arch 2020 can be launched from both black hole (e.g. Rezzolla et al. 2011) and NS (e.g. Metzger, Quataert & Thompson 2008) remnants of compact binary coalescences, as necessitated by the ‘relativistic fireball’ model of prompt GRB emission (e.g. Piran 1999; Lee & Ramirez-Ruiz 2007; Nakar 2007).”
• Multi-messenger observations of a binary neutron star merger (2017, background): “In 2005, the field of short gamma-ray burst (sGRB) studies experienced a breakthrough (for reviews see Nakar 2007; Berger 2014) with the identification of the first host galaxies of sGRBs and multi-wavelength observation (from X-ray to optical and radio) of their afterglows (Berger et al. 2005; Fox…”