Prompt gamma-ray burst emission from gradual magnetic dissipation

Paz Beniamini, Dimitrios Giannios

Research output: Contribution to journalArticlepeer-review


We considered a model for the prompt phase of gamma-ray burst emission arising from a magnetized jet undergoing gradual energy dissipation due to magnetic reconnection. The dissipated magnetic energy is translated to bulk kinetic energy and to acceleration of particles. The energy in these particles is released via synchrotron radiation as they gyrate around the strong magnetic fields in the jet. At small radii, the optical depth is large, and the radiation is reprocessed through Comptonization into a narrow, strongly peaked component. At larger distances the optical depth becomes small and radiation escapes the jet with a non-thermal distribution. The obtained spectra typically peak around ≈300 keV (as observed) and with spectral indices below and above the peak that are, for a broad range of the model parameters, close to the observed values. The small radius of dissipation causes the emission to become self-absorbed at a few keV and can sufficiently suppress the optical and X-ray fluxes within the limits required by observations .

Original languageEnglish
Pages (from-to)3202-3211
Number of pages10
JournalMonthly Notices of the Royal Astronomical Society
Issue number3
StatePublished - 1 Jul 2017
Externally publishedYes

Bibliographical note

Publisher Copyright:
© 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.


  • General
  • Magnetic reconnection
  • Non-thermal-radiation mechanisms
  • Radiation mechanisms
  • Thermal-gamma-ray burst


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