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Properties of magnetic turbulence in GRB afterglows

Published online by Cambridge University Press:  30 October 2024

Evgeny Derishev Open the ORCID record for Evgeny Derishev [Opens in a new window]
Evgeny Derishev*
Affiliation:
Institute of Applied Physics, Nizhny Novgorod, Russia
*
Email: derishev@appl.sci-nnov.ru
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Abstract

We present a model-independent way to characterise properties of the magnetic-field turbulence in the emitting regions of Gamma-Ray Burst afterglows. Our only assumption is that afterglows’ synchrotron radiation is efficient. It turns out that the gyroradius of plasma particles must be smaller (with a good margin) than the correlation length of the magnetic-field fluctuations. Such turbulence is essentially non-linear and therefore must be produced by some kind of magnetohydrodynamical instability, likely acting on top of kinetic Weibel instability. We also find that the emitting particles are loosely confined to local magnetic-field structures and diffusion allows them to sample the entire distribution of local magnetisation values. This means that one-zone approach to modelling the afterglow spectra is still valid despite the non-linear nature of the magnetic turbulence. However, the non-linear turbulence may (and likely will) change the synchrotron spectrum of individual electrons.

Keywords

gamma-ray burstgeneralradiation mechanismsnon-thermalturbulencemagnetic fields
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 41 , 2024 , e081
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of Astronomical Society of Australia

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