Remnants from Gamma-Ray Bursts

Abstract

We model the intermediate time evolution of a "jetted" gamma-ray burst by two blobs of matter colliding with the interstellar medium. We follow the hydrodynamical evolution of this system numerically and calculate the bremsstrahlung and synchrotron images of the remnant. We find that for a burst energy of $10^{51}$ erg the remnant becomes spherical after $\sim 5000$ years when it collects $\sim 50M_{\odot }$ of interstellar mass. This result is independent of the exact details of the GRB, such as the opening angle. After this time a gamma-ray burst remnant has an expanding sphere morphology. The similarity to a supernova remnant makes it difficult distinguish between the two at this stage. The expected number of non-spherical gamma-ray burst remnants is $\sim 0.05$ per galaxy for a beaming factor of 0.01 and a burst energy of $10^{51}$ erg. Our results suggest that that the double-shell object DEM L 316 is not a GRB remnant.

16 pages, 9 figures, Substantial revisions, Accepted by ApJ

References in corpus (4)

• Luminosities and Space Densities of Gamma-Ray Bursts
• On the Kinematic Origin of the Luminosity-Pulse Lag Relationship in Gamma-ray Bursts
• Post Newtonian SPH
• GRB990510: on the possibility of a beamed X-ray afterglow

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