Short-Duration Gamma-Ray Bursts

By E. Berger. 2013

943 citations recorded by the source corpus.

Gamma-ray bursts (GRBs) display a bimodal duration distribution with a separation between the short- and long-duration bursts at about 2 s. The progenitors of long GRBs have been identified as massive stars based on their association with Type Ic core-collapse supernovae (SNe), their exclusive location in star-forming galaxies, and their strong correlation with bright UV regions within their host galaxies. Short GRBs have long been suspected on theoretical grounds to arise from compact object binary mergers (neutron star–neutron star or neutron star–black hole). The discovery of short GRB afterglows in 2005 provided the first insight into their energy scale and environments, as well as established a cosmological origin, a mix of host-galaxy types, and an absence of associated SNe. In this review, I summarize nearly a decade of short GRB afterglow and host-galaxy observations and use this information to shed light on the nature and properties of their progenitors, the energy scale and collimation of the re...

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/c7efeea8d515f06761e1d4765e71a95a0ebe0a0d

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Citations in the corpus

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…”
Tidal Deformability from GW170817 as a Direct Probe of the Neutron Star Radius (2018, background): “…star mergers as the sources of at least some short-duration gamma-ray bursts, as has long been theorized (Eichler et al. 1989; Narayan et al. 1992; Berger 2014), as well as the source of kilonovae, predicted to be powered by the radioactive decay of merger ejecta (Li & Paczyński 1998; Metzger et…”
Fast Radio Bursts from Magnetars Born in Binary Neutron Star Mergers and Accretion Induced Collapse (2019, background): “The consistency of these predictions with the observed host galaxy demographics and spatial offset distributions of SGRBs provided strong evidence for the association of SGRBs with BNS mergers (Berger 2014), even prior to the discovery of GW170817 (Abbott et al. 2017b, 2017a).”
The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. V. Rising X-Ray Emission from an Off-axis Jet (2017, background): “…environments and properties of emission of SGRBs in the past decade provided solid indirect evidence of the association of SGRBs with BNS mergers (Fong & Berger 2013; Berger 2014; Fong et al. 2015), thus motivating our search for observational signatures of on-axis and off-axis jets in GW170817.”
The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. III. Optical and UV Spectra of a Blue Kilonova from Fast Polar Ejecta (2017, background): “…of short gamma-ray bursts (SGRBs) based on both theoretical viability (Eichler et al. 1989; Narayan et al. 1992) and observations of their X-ray, optical and radio afterglows (Berger 2014; Berger et al. 2005; Fox et al. 2005; Hjorth et al. 2005; Soderberg et al. 2006; Fong et al. 2013, 2015).”
The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. VI. Radio Constraints on a Relativistic Jet and Predictions for Late-time Emission from the Kilonova Ejecta (2017, background): “In particular, these observations point to lowdensity environments of ~ - –10 0.13 cm−3, and typical beaming-corrected energies of ~ –10 1049 50 erg (Berger 2014; Fong et al. 2015).”
Double neutron stars: merger rates revisited (2017, background): “However, NS-NS mergers are only one of the possible sGRB progenitors and currently other candidates (BHNS mergers) cannot be excluded (e.g. Berger 2014).”
The Origin of r-process Elements in the Milky Way (2017, background): “For comparison with other observational constraints such as short-duration gamma-ray bursts (Berger 2014) and gravitational wave measurements (Abbott et al. 2016), a calculation of cosmological NS-NS merger rate densities is required.”
Off-axis emission of short γ-ray bursts and the detectability of electromagnetic counterparts of gravitational-wave-detected binary mergers (2016, background): “1 IN T RO D U C T I O N Short-duration gamma-ray bursts (SGRBs) are expected to be associated with the merger of a compact binary system in which at least one of the two components is a neutron star (NS), the other possibly being a black hole (BH; Eichler et al. 1989; Nakar 2007; Berger 2014).”
Dynamical Mass Ejection from Binary Neutron Star Mergers (2016, background): “About 10% of all observed SGRBs show offsets larger than 20 kiloparsecs from the bulge of their host galaxies (Berger et al. 2005; Berger 2014).”
Characterizing the Fast Radio Burst Host Galaxy Population and its Connection to Transients in the Local and Extragalactic Universe (2021, background): “…yr −1 and 11.7 Me yr −1 for the hosts of Type Ia ULXsa Kovlakas et al. (2020) SGRBs Leibler & Berger (2010), Fong et al. (2010), Fong & Berger (2013), Berger (2014) LGRBs Blanchard et al. (2016), Taggart & Perley (2021) CCSNe Schulze et al. (2020) SLSNe Schulze et al. (2020), Taggart & Perley…”
The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. I. Discovery of the Optical Counterpart Using the Dark Energy Camera (2017, background): “…mechanisms for GW sources has been proposed over the years (Metzger & Berger 2012), including short-duration GRBs (Eichler et al. 1989; Nakar 2007; Berger 2014), on- or off-axis afterglow emission from radio to X-rays (van Eerten & MacFadyen 2011; Coward et al. 2014; Fong et al. 2015; Lamb &…”
THE LIGHT CURVE OF THE MACRONOVA ASSOCIATED WITH THE LONG–SHORT BURST GRB 060614 (2015, background): “For the macronovae at z ≥ 0.4, HST observations are crucial to get the signal but HST observations of such “high”-z short GRBs were very rare (Berger 2014).”
The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. VII. Properties of the Host Galaxy and Constraints on the Merger Timescale (2017, background): “We note that ≈75%–80% of short GRBs occur in fainter regions of their hosts than GW170817 (Fong et al. 2017).”
The birth of black holes: neutron star collapse times, gamma-ray bursts and fast radio bursts (2014, background): “Gamma-ray bursts (GRBs) with short durations ( 2 s) and hard spectra are associated with the coalescences of compact object binaries, i.e. either NS–NS or NS–black hole mergers (Lee & RamirezRuiz 2007; Nakar 2007; Berger 2013).”
On the formation history of Galactic double neutron stars (2018, background): “…beyond the Milky Way to cosmological distances, but inference from these is complicated by the difficulty of measuring jet opening angles and uncertain selection effects, and relies on the additional assumption of a one-to-one correspondence between short GRBs and DNS mergers (Berger 2014).”