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The association of GRB 060218 with a supernova and the evolution of the shock wave
A supernova is caught in the act of exploding, directly observing the shock break-out, which indicates that the GRB progenitor was a Wolf–Rayet star.
Low-Luminosity Gamma-Ray Bursts as a Unique Population: Luminosity Function, Local Rate, and Beaming Factor
Swift BAT has detected ~200 long-duration GRBs, with redshift measurements for ~50 of them. We derive the luminosity function (?HL) and the local event rate (?) of the conventional high-luminosity
Afterglow Emission from Highly Collimated Jets with Flat Electron Spectra: Application to the GRB 010222 Case?
We derive light curves of the afterglow emission from highly collimated jets if the power-law index (p )o f the electron energy distribution is above 1 but below 2. We find the following: (1) Below
The Observer's Guide to the Gamma-Ray Burst-Supernova Connection
We present a detailed report of the connection between long-duration gamma-ray bursts (GRBs) and their accompanying supernovae (SNe). The discussion presented here places emphasis on how
X-ray Flares from Postmerger Millisecond Pulsars
This work shows that x-ray flares discovered in two short gamma-ray bursts last much longer than the previously proposed postmerger energy-release time scales and can be produced by differentially rotating, millisecond pulsars after the mergers of binary neutron stars.
Gamma-ray burst afterglows: effects of radiative corrections and non-uniformity of the surrounding medium
The afterglow of a gamma-ray burst (GRB) is commonly thought to be the result of continuous deceleration of a relativistically expanding fireball in the surrounding medium. Assuming that the
Gamma-ray bursts and afterglows from rotating strange starsand neutron stars
We here discuss a new model of $\gamma$-ray bursts (GRBs) based on differentially rotating strange stars. Strange stars in this model and differentially rotating neutron stars in the
Overall Evolution of Jetted Gamma-ray Burst Ejecta
Whether gamma-ray bursts are highly beamed or not is a very difficult but important problem that we are confronted with. Some theorists suggest that beaming effect usually leads to a sharp break in
The afterglow of GRB 990123 and a dense medium
Recent observations show that the temporal decay of the R-band afterglow from GRB 990123 steepened about 2.5 days after the burst. We here propose a possible explanation for such a steepening: a
The conventional generic model is deemed to explain the dynamics of $\gamma$-ray burst remnants very well, no matter whether they are adiabatic or highly radiative. However, we find that for