Short-hard gamma-ray bursts

  title={Short-hard gamma-ray bursts},
  author={Ehud Nakar},
  journal={Physics Reports},
  • E. Nakar
  • Published 25 January 2007
  • Physics
  • Physics Reports
Short-Duration Gamma-Ray Bursts
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
Long-duration gamma-ray bursts (GRBs) and X-ray flashes (XRFs) are produced by highly relativistic jets ejected in core-collapse supernova (SN) explosions. The origin of short hard gamma-ray bursts
High-energy γ-ray emission from gamma-ray bursts — before GLAST
Gamma-ray bursts (GRBs) are short and intense emission of soft γ-rays, which have fascinated astronomers and astrophysicists since their unexpected discovery in 1960s. The X-ray/optical/radio
Bimodal Long-lasting Components in Short Gamma-Ray Bursts: Promising Electromagnetic Counterparts to Neutron Star Binary Mergers
Long-lasting emission of short gamma-ray bursts (GRBs) is crucial to reveal the physical origin of the central engine as well as to detect electromagnetic (EM) counterparts to gravitational waves
In an effort to understand the puzzle of classifying gamma-ray bursts (GRBs), we perform a systematic study of Swift GRBs and investigate several short GRB issues. Though short GRBs have a short (≲ 2
Gamma-ray burst overview
Since its launch on 20 November 2004, the Swift mission has detected ∼100 gamma-ray bursts (GRBs) each year, and immediately (within ∼90 s) started x-ray and UV/optical observations of the afterglow.
Constraints on long-lived remnants of neutron star binary mergers from late-time radio observations of short duration gamma-ray bursts
The coalescence of a binary neutron star (NS) system may in some cases produce a massive NS remnant that is long-lived and, potentially, indefinitely stable to gravitational collapse. Such a remnant
Swift observations of gamma-ray bursts
  • N. Gehrels
  • Physics
    Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences
  • 2007
The detection of X-ray afterglows has led to accurate localizations and the conclusion that short GRBs can occur in non-star-forming galaxies or regions, whereas long GRBs are strongly concentrated within the star-forming regions.


Discovery of the short γ-ray burst GRB 050709
Gamma-ray bursts (GRBs) fall into two classes: short-hard and long-soft bursts. The latter are now known to have X-ray and optical afterglows, to occur at cosmological distances in star-forming
The afterglow of GRB 050709 and the nature of the short-hard γ-ray bursts
The final chapter in the long-standing mystery of the γ-ray bursts (GRBs) centres on the origin of the short-hard class of bursts, which are suspected on theoretical grounds to result from the
The afterglow and elliptical host galaxy of the short γ-ray burst GRB 050724
Despite a rich phenomenology, γ-ray bursts (GRBs) are divided into two classes based on their duration and spectral hardness—the long-soft and the short-hard bursts. The discovery of afterglow
A short γ-ray burst apparently associated with an elliptical galaxy at redshift z = 0.225
Gamma-ray bursts (GRBs) come in two classes: long (> 2 s), soft-spectrum bursts and short, hard events. Most progress has been made on understanding the long GRBs, which are typically observed at
Short Gamma-Ray Bursts and Mergers of Compact Objects: Observational Constraints
Gamma-ray burst (GRB) data accumulated over the years have shown that the distribution of their time duration is bimodal. While there is some evidence that long bursts are associated with
Detection of a γ-ray burst of very long duration and very high energy
ALTHOUGH γ-ray bursts (GRBs) have been known for more than 20 years, their origin remains mysterious1. Suggestions have ranged from nearby colliding comets2 to merging neutron stars at cosmological
The Afterglows and Host Galaxies of Short GRBs: An Overview
Despite a rich diversity in observational properties, gamma-ray bursts (GRBs) can be divided into two broad categories based on their duration and spectral hardness -- the long-soft and the
An origin in the local Universe for some short γ-ray bursts
Gamma-ray bursts (GRBs) divide into two classes: ‘long’, which typically have initial durations of T90 > 2 s, and ‘short’, with durations of T90 < 2 s (where T90 is the time to detect 90% of the
BATSE Observations of Gamma-Ray Burst Tails
With the discovery of low-energy radiation appearing to come from the site of gamma-ray bursts in the hours to weeks after the initial burst of gamma rays, it would appear that astronomers have seen
X-ray flares following short gamma-ray bursts from shock heating of binary stellar companions
The discovery of long-lasting (~100 s) X-ray flares following short gamma-ray bursts initially called into question whether they were truly classical short-hard bursts. Opinion over the last few