Skip banner and navigation tools.

 |  site map

Skip sidebars of related page links.

Pre-Swift Gamma-Ray Bursts

Gamma-Ray Bursts (GRBs) are the most explosive events in the Universe since the Big Bang. For the short time that they are visible, they outshine the rest of the gamma-ray sky. The energy each burst emits may be up to 1054 erg (where 107 erg is 1 joule) if the emission is isotropic; if the radiation is beamed towards us, then the total energy is reduced by a factor of (solid angle of beam)/4π.

GRB animation
A GRB detected by BATSE, the Burst And Transient Source Experiment, on-board the Compton Gamma-Ray Observatory (CGRO).


GRBs were first discovered accidentally in the late 1960s by the Vela satellites. These satellites belonged to the United States Air Force and were launched as part of an effort to enforce the new nuclear test ban treaty. This treaty prohibited the testing of nuclear devices in the atmosphere or space and the Vela satellites were designed to monitor any such explosions. However, rather than identifying any illegal testing, the satellites detected non-terrestrial gamma-ray events - i.e., from outside our atmosphere - and, so, GRBs were discovered.

Between 1991 and 2000, BATSE detected 2704 GRBs, as shown in the diagram below. It can be seen that they are fairly uniformly spread over the entire sky, indicating that they are either nearby and clustered around our position, or they do not originate in our own Galaxy. In 1997, BeppoSAX detected the first X-ray afterglow within a GRB error box (GRB970228). An optical transient was also found, fading within a week (HST press release). The identification of GRB970228 with a host galaxy at a known distance (redshift of 0.695) confirmed the cosmological origin of GRBs.

Bursts detected by BATSE

Long duration, bright bursts are shown in red, while shorter, weak bursts appear in purple. The bursts in grey are those for which the fluence could not be calculated, because of incomplete data. (The fluence indicates the total energy passing through a unit area; in X-ray astronomy, the unit of fluence is erg cm-2.)


GRBs last between a few milliseconds and several minutes. There appear to be two populations, 'short' bursts, with durations peaking around 0.3 seconds and 'long' bursts, which last around 30 seconds, with the 'dividing line' between the groups being ~ 2 seconds.

GRB durations
Durations of GRBs detected by BATSE. Peaks in the number of bursts detected can be seen around 0.3 and 30 seconds.


It is thought that the long and short bursts may be formed through two different methods:

The Fireball Model

Regardless of the progenitor, the favoured model for GRBs is the Fireball Model, in which the emission is separated into 2 components: the prompt outburst phase (strong gamma-ray and X-ray emission) due to internal shocks in the relativistic blast-wave, followed by the afterglow (strong X-ray, optical and radio emission) which arises from the cooling fireball and its interaction with the surrounding medium.

Fireball model

Why Swift?

Before the launch of Swift, only longer bursts have been investigated, since commands had to be sent to the relevant satellite to point it in the correct direction, which this takes time. Swift is designed to be much more autonomous and, when it has detected gamma-rays, automatically slews to the position of the GRB within seconds.

Although the initial emission appears at gamma-ray energies, many bursts are also detected in the X-ray, optical and radio bands - the so-called afterglow emission. Swift is a multi-wavelength mission, with three instruments on-board - the BAT (Burst Alert Telescope), XRT (X-ray Telescope) and UVOT (Ultraviolet and Optical Telescope) - enabling the study of the initial burst and afterglow emission over a broad range of wavelengths. After a GRB has been detected and localised, follow-up observations with ground-based telescopes can occur. Among these are included the Faulkes and Liverpool robotic telescopes.