Abstract
Gamma-Ray Bursts (GRBs) are the strongest explosions in the Universe, which due to their extreme character likely involve some of the strongest magnetic fields in nature. This review discusses the possible roles of magnetic fields in GRBs, from their central engines, through the launching, acceleration and collimation of their ultra-relativistic jets, to the dissipation and particle acceleration that power their \(\gamma\)-ray emission, and the powerful blast wave they drive into the surrounding medium that generates their long-lived afterglow emission. An emphasis is put on particular areas in which there have been interesting developments in recent years.
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Notes
These plateaus have several alternative explanation, which are at least as compelling as the magnetar explanation, such as promptly ejected slow material that gradually catches up with the afterglow shock (Nousek et al. 2006; Granot and Kumar 2006), time-varying afterglow shock microphysical parameters (Granot et al. 2006), viewing angle effects (Eichler and Granot 2006), or a two-component jet (Peng et al. 2005; Granot et al. 2006).
A failed jet produces, most likely, a low-luminosity GRB when a shock wave generated by the dissipated energy breaks out from the seller envelope.
This analysis does not account for 3D effects that can slow down the head’s propagation speed (Bromberg and Tchekhovskoy 2015).
http://gammaray.msfc.nasa.gov/batse/grb/catalog/current/ from April 21, 1991 until August 17, 2000.
http://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html, from July 17, 2008 until February 14, 2014.
http://swift.gsfc.nasa.gov/archive/grb_table/, from December 17, 2004 until February 14, 2014.
The confidence level is defined here as \(\int_{0}^{{\chi^{2}}}P(x,\nu)dx\), where \(P(\chi^{2},\nu)\) is the probability density function of \(\chi^{2}\) with \(\nu\) degrees of freedom (Press et al. 1992).
Or possibly even a dominant photospheric component in the case of GRB 090902B.
The magnetic field in the jet’s frame is \(B'=B/\varGamma\), where \(\varGamma\) is its bulk Lorentz factor.
In an alternative scenario, the afterglow emission is dominated at early times by the contribution of a long-lived reverse shock (Uhm and Beloborodov 2007; Genet et al. 2007), which allows to reproduce more easily the observed diversity and variability, such as X-ray plateaus (Uhm et al. 2012; Hascoët et al. 2014) or X-ray flares (Hascoet et al. 2015), though in this scenario a transition to forward shock dominance is expected at late times but not observed.
It is usually also further assumed that practically all of the electrons take part in this acceleration process and form such a non-thermal (power-law) distribution, leaving no thermal component (which is not at all clear or justified; e.g. Eichler and Waxman 2005).
The exact numerical coefficient depends on the exact assumptions, and in particular on whether the acceleration time is assumed to be a fraction of or a complete Larmor gyration time, which is in any case a very fast acceleration, and arguably even unrealistically so. Here \(\alpha\approx1/137\) is the fine structure constant.
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Acknowledgements
The authors acknowledge support from the ISF grant 719/14 (JG), as well as from the I-CORE Program—ISF grant 1829/12, the ISA grant 3-10417, and an ISF-CNSF grant (TP).
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Granot, J., Piran, T., Bromberg, O. et al. Gamma-Ray Bursts as Sources of Strong Magnetic Fields. Space Sci Rev 191, 471–518 (2015). https://doi.org/10.1007/s11214-015-0191-6
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DOI: https://doi.org/10.1007/s11214-015-0191-6