The effect of magnetic fields on γ-ray bursts inferred from multi-wavelength observations of the burst of 23 January 1999

Galama, T. J.; Briggs, M. S.; Wijers, R. A. M. J.; Vreeswijk, P. M.; Rol, E.; Paradijs, J. van; Kouveliotou, C.; Preece, R.; Bremer, M.; Smith, I. A.; Tilanus, R. P. J.; Bruyn, A. G. de; Strom, R. G.; Pooley, G. G.; Castro-Tirado, A. J.; Tanvir, N. R.; Robinson, C. R.; Hurley, K.; Heise, J.; Telting, J. H.; Rutten, R. G. M.; Packham, C.; Swaters, Robert A.; Davies, J. K.; Fassia, A.; Green, S. F.; Foster, Michael J.; Sagar, Ram; Pandey, A. K.; Nilakshi,; Yadav, R. K. S.; Ofek, E. O.; Leibowitz, E. M.; Ibbetson, P.; Rhoads, James E.; Falco, E.; Petry, C. E.; Impey, C.; Geballe, T. R.; Bhattacharya, Dipankar

doi:10.1038/18828

Cited by 128 publications

(109 citation statements)

References 23 publications

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“…The late-time afterglow observations show a more gradual decline Kulkarni et al 1999b;Castro-Tirado et al 1999;Fruchter et al 1999;Sari & Piran 1999b) (see Figure 10). Galama et al (1999) have shown, that if one assumes that the emission detected by ROTSE comes from a non-relativistic source of size ct, then the observed brightness temperature T b 10 17 K of the optical flash exceeds the Compton limit of 10 12 K. This confirms the highly relativistic nature of the GRB source.…”

Section: The Reverse Shock Emissionsupporting

confidence: 61%

Gamma Ray Bursts and Their Afterglows

Sari

2006

AIP Conference Proceedings

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Abstract. Gamma-Ray Bursts are extreme astrophysical events, which emit the bulk of their energy as photons in the 0 1 1 0 MeV range, and whose durations span milliseconds to tens of minutes. They are formed in extreme relativistic outflows with Lorentz factors of hundreds, and reside at cosmological distances. They are followed by X-ray, optical and radio afterglows which can be observed for over a year after the event. Observations of afterglows showed that the emission is from jets, and when corrected for this geometry the energies of GRBs appear to cluster around 5 ¢ 10 50 erg -very comparable to that of supernovae. Evidence in the last several years shows that a significant fraction of long GRBs are related to a peculiar type of supernova explosions. These supernovae most likely mark the birth events of stellar mass black holes as the final products of the evolution of very massive stars. Short bursts are still somewhat mysterious, but it is known that some of them are produced by an old population of stars. Neutron star merger is a leading candidate as the progenitor of short GRBs.

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Section: The Reverse Shock Emissionsupporting

confidence: 61%

Gamma Ray Bursts and Their Afterglows

Sari

2006

AIP Conference Proceedings

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“…However, if the maximum source size ct results in a brightness temperature that exceeds the inverseCompton limit TB ≈ 10 12 K in the rest-frame, then this assumption is wrong and the GRB outflow is likely relativistic. Given that Iν /ν 3 (where Iν is the specific intensity) is a relativistic invariant (Mihalas & Mihalas 1984), the observed brightness temperature is related to the minimum Lorentz factor such that T b /TB = Γ 3 (see similar arguments made by Kulkarni et al 1998;Galama et al 1999).…”

Section: Brightness Temperature and Minimum Lorentz Factormentioning

confidence: 99%

The Arcminute Microkelvin Imager catalogue of gamma-ray burst afterglows at 15.7 GHz

Anderson

Staley

Horst

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present the Arcminute Microkelvin Imager (AMI) Large Array catalogue of 139 gamma-ray bursts (GRBs). AMI observes at a central frequency of 15.7 GHz and is equipped with a fully automated rapid-response mode, which enables the telescope to respond to highenergy transients detected by Swift. On receiving a transient alert, AMI can be on-target within two minutes, scheduling later start times if the source is below the horizon. Further AMI observations are manually scheduled for several days following the trigger. The AMI GRB programme probes the early-time (< 1 day) radio properties of GRBs, and has obtained some of the earliest radio detections (GRB 130427A at 0.36 and GRB 130907A at 0.51 days post-burst). As all Swift GRBs visible to AMI are observed, this catalogue provides the first representative sample of GRB radio properties, unbiased by multi-wavelength selection criteria. We report the detection of six GRB radio afterglows that were not previously detected by other radio telescopes, increasing the rate of radio detections by 50% over an 18-month period. The AMI catalogue implies a Swift GRB radio detection rate of 15%, down to ∼ 0.2 mJy/beam. However, scaling this by the fraction of GRBs AMI would have detected in the Chandra & Frail sample (all radio-observed GRBs between 1997 − 2011), it is possible ∼ 44 − 56% of Swift GRBs are radio bright, down to ∼ 0.1 − 0.15 mJy/beam. This increase from the Chandra & Frail rate (∼ 30%) is likely due to the AMI rapid-response mode, which allows observations to begin while the reverse-shock is contributing to the radio afterglow.

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“…We have fit the NIR/optical data (Castro Tirado 1999;Fruchter et al 1999;Galama et al 1999;Holland et al 2000;Kulkarni et al 1999a) and the radio data (Galama et al 1999;Kulkarni et al 1999b) for this GRB. In Fig.…”

Section: Grb 990123mentioning

confidence: 99%

On the radio afterglow of gamma ray bursts

Dado

Dar

Rújula

2003

A&A

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Abstract. We use the cannonball (CB) model of gamma ray bursts (GRBs) to predict the spectral and temporal behaviour of their radio afterglows (AGs). A single simple expression describes the AGs at all times and frequencies; its high-frequency limit reproduces the successful CB model predictions for optical and X-ray AGs. We analyze all of the observed radio AGs of GRBs with known redshifts, including those of the exceptionally close-by GRB 980425. We also study in detail the timeevolution of the AGs' spectral index. The agreement between theory and observations is excellent, even though the CB model is extremely frugal in the number of parameters required to explain the radio observations. We propose to use the scintillations in the radio AGs of GRBs to verify and measure the hyperluminal speed of their jetted CBs, whose apparent angular velocity is of the same order of magnitude as that of galactic pulsars, consistently measured directly, or via scintillations.

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The effect of magnetic fields on γ-ray bursts inferred from multi-wavelength observations of the burst of 23 January 1999

Cited by 128 publications

References 23 publications

Gamma Ray Bursts and Their Afterglows

Gamma Ray Bursts and Their Afterglows

The Arcminute Microkelvin Imager catalogue of gamma-ray burst afterglows at 15.7 GHz

On the radio afterglow of gamma ray bursts

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