Magnetic flare model of gamma-ray bursts

Details Magnetic flare model of gamma-ray bursts Magnetic flare model of gamma-ray bursts

Jul 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984natur.310..121l&link_type=abstract

Nature (ISSN 0028-0836), vol. 310, July 12, 1984, p. 121, 122.

Physics

11

Gamma Ray Bursts, Neutron Stars, Stellar Flares, Synchrotron Radiation, Electromagnetic Radiation, Magnetohydrodynamic Waves, Raman Spectra, Stellar Magnetic Fields, Stellar Structure

Scientific paper

The thermal synchrotron (TS) interpretation of gamma-ray burst continuum spectra requires an emission region which is hot, optically thin, and possessed of a super-Eddington flux of 10 to the 30 ergs/sq cm per sec for a 10-km neutron star. In order to maintain a pair population close to the Maxwellian, the collision excitation rate into higher Landau levels must exceed the cyclotron decay rates. Even if collective processes whose rates are close to the electron plasma frequency, or scattering by heavy ions, are invoked, a particle density of 10 to the 25th/cu cm is still needed. Both hypotheses point in the direction of a dense but thin emitting sheet, to whose structure attention is presently given together with the generation, propagation and coupling of the electromagnetic energy fluxes. A flare-like model can account for most of gamma ray bursts' general features.

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