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39 - A GRB simulation using 3-D relativistic hydrodynamics

Published online by Cambridge University Press:  11 August 2009

By
J. K. Cannizzo ,
N. Gehrels  and
E. T. Vishniac
Edited by
Peter Höflich ,
Pawan Kumar  and
J. Craig Wheeler
J. K. Cannizzo
Affiliation:
NASA/GSFC/Lab. for High Energy Astrophysics/Code 661, Greenbelt, MD 20771; also University of Maryland Baltimore County
N. Gehrels
Affiliation:
NASA/GSFC/Lab. for High Energy Astrophysics/Code 661, Greenbelt, MD 20771
E. T. Vishniac
Affiliation:
Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21210
Peter Höflich
Affiliation:
University of Texas, Austin
Pawan Kumar
Affiliation:
University of Texas, Austin
J. Craig Wheeler
Affiliation:
University of Texas, Austin
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Summary

Abstract

We present the first unrestricted, three-dimensional relativistic hydrodynamical calculations of the blob of gas associated with the jet producing a gamma-ray burst as applied to the time when afterglow radiation is produced. Our main findings are that (ⅰ) gas ahead of the advancing blob does not accrete onto and merge with the blob material but rather flows around the blob, (ⅱ) the decay light curve steepens at a time corresponding roughly to γ˗1 ≈ θ (in accord with earlier studies), and (ⅲ) the rate of decrease of the forward component of momentum in the blob is well-fit by a simple model in which the gas in front of the blob exerts a drag force on the blob, and the cross sectional area of the blob increases quadratically with laboratory time.

Introduction

Gamma-ray bursts are the most powerful explosions in the Universe. If GRBs were isotropic, then the measured redshifts would imply total explosion energies of ∼1052–1054 ergs (Frail et al. 2001). Theoretical work on relativistic jet expansion, however, shows that one expects a steepening in the decay light curve if one is looking down the axis of a jet as the flow decelerates from a bulk Lorentz factor γ˗1 < θ to γ˗1 > θ, where θ is the jet beaming angle (Rhoads 1999). The concept of a “break” corresponding to γ˗1 ≃ θ has been used to infer the presence of strong beaming in GRBs (Frail et al.

Type
Chapter
Information
Cosmic Explosions in Three Dimensions
Asymmetries in Supernovae and Gamma-Ray Bursts
 , pp. 346 - 350
Publisher: Cambridge University Press
Print publication year: 2004

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References

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  • A GRB simulation using 3-D relativistic hydrodynamics
    • By J. K. Cannizzo, NASA/GSFC/Lab. for High Energy Astrophysics/Code 661, Greenbelt, MD 20771; also University of Maryland Baltimore County, N. Gehrels, NASA/GSFC/Lab. for High Energy Astrophysics/Code 661, Greenbelt, MD 20771, E. T. Vishniac, Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21210
  • Edited by Peter Höflich, University of Texas, Austin, Pawan Kumar, University of Texas, Austin, J. Craig Wheeler, University of Texas, Austin
  • Book: Cosmic Explosions in Three Dimensions
  • Online publication: 11 August 2009
  • Chapter DOI: https://doi.org/10.1017/CBO9780511536236.039
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  • A GRB simulation using 3-D relativistic hydrodynamics
    • By J. K. Cannizzo, NASA/GSFC/Lab. for High Energy Astrophysics/Code 661, Greenbelt, MD 20771; also University of Maryland Baltimore County, N. Gehrels, NASA/GSFC/Lab. for High Energy Astrophysics/Code 661, Greenbelt, MD 20771, E. T. Vishniac, Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21210
  • Edited by Peter Höflich, University of Texas, Austin, Pawan Kumar, University of Texas, Austin, J. Craig Wheeler, University of Texas, Austin
  • Book: Cosmic Explosions in Three Dimensions
  • Online publication: 11 August 2009
  • Chapter DOI: https://doi.org/10.1017/CBO9780511536236.039
Available formats
×

Save book to Google Drive

To save content items to your account, please confirm that you agree to abide by our usage policies. If this is the first time you use this feature, you will be asked to authorise Cambridge Core to connect with your account. Find out more about saving content to Google Drive.

  • A GRB simulation using 3-D relativistic hydrodynamics
    • By J. K. Cannizzo, NASA/GSFC/Lab. for High Energy Astrophysics/Code 661, Greenbelt, MD 20771; also University of Maryland Baltimore County, N. Gehrels, NASA/GSFC/Lab. for High Energy Astrophysics/Code 661, Greenbelt, MD 20771, E. T. Vishniac, Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21210
  • Edited by Peter Höflich, University of Texas, Austin, Pawan Kumar, University of Texas, Austin, J. Craig Wheeler, University of Texas, Austin
  • Book: Cosmic Explosions in Three Dimensions
  • Online publication: 11 August 2009
  • Chapter DOI: https://doi.org/10.1017/CBO9780511536236.039
Available formats
×