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Photospheric Emission of Gamma-Ray Bursts

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Abstract

We review the physics of GRB production by relativistic jets that start highly opaque near the central source and then expand to transparency. We discuss dissipative and radiative processes in the jet and how radiative transfer shapes the observed nonthermal spectrum released at the photosphere. A comparison of recent detailed models with observations gives estimates for important parameters of GRB jets, such as the Lorentz factor and magnetization. We also discuss predictions for GRB polarization and neutrino emission.

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Notes

  1. The photospheric shock breakout should not be confused with the jet breakout from the progenitor star. The jet breakout occurs at smaller radii and huge optical depths.

  2. A different hadronic shock model explanation was also proposed by Asano et al. (2010).

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Acknowledgements

AMB’s research is supported by NSF grant AST-1412485, NASA grant NNX15AE26G, and a grant from the Simons Foundation (#446228, Andrei Beloborodov). PM’s research is supported by NASA grant NNX13AH50G.

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Authors and Affiliations

  1. Physics Department and Columbia Astrophysics Laboratory, Columbia University, 538 West 120th Street, New York, NY, 10027, USA

    A. M. Beloborodov

  2. Center for Particle and Gravitational Astrophysics, Dept. of Astronomy & Astrophysics, Pennsylvania State University, University Park, PA, 16802, USA

    P. Mészáros

  3. Center for Particle and Gravitational Astrophysics, Dept. of Physics, Pennsylvania State University, University Park, PA, 16802, USA

    P. Mészáros

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  1. A. M. Beloborodov
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  2. P. Mészáros
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Correspondence to A. M. Beloborodov.

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Beloborodov, A.M., Mészáros, P. Photospheric Emission of Gamma-Ray Bursts. Space Sci Rev 207, 87–110 (2017). https://doi.org/10.1007/s11214-017-0348-6

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