Synchrotron cooling and annihilation of an e/+/-e/-/ plasma - The radiation mechanism for the 5 March, 1979 transient

Details Synchrotron cooling and annihilation of an e/+/-e/-/ plasma - The radiation mechanism for the 5 March, 1979 transient Synchrotron cooling and annihilation of an e/+/-e/-/ plasma - The radiation mechanism for the 5 March, 1979 transient

Mar 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981ap%26ss..75..193r&link_type=abstract

(Symposium on Cosmic Gamma-Ray Bursts, Toulouse, France, Nov. 26-29, 1979.) Astrophysics and Space Science, vol. 75, no. 1, Mar.

Astronomy and Astrophysics

Astronomy

67

Annihilation Reactions, Bursts, Electron Plasma, Electron-Positron Plasmas, Gamma Ray Astronomy, Neutron Stars, Radiant Cooling, Synchrotron Radiation, Astronomical Models, Electron-Positron Pairs, Energy Spectra, Gamma Ray Spectra, Magellanic Clouds, Positrons, Stellar Atmospheres, Supernova Remnants, Transient Oscillations

Scientific paper

Positron-electron pair radiation is examined as a mechanism that could be responsible for the impulsive phase emission of the 5 March, 1979 transient. Synchrotron cooling and subsequent annihilation of the pairs can account for the energy spectrum, the very high brightness, and the 0.4 MeV feature observed from this transient, whose source is likely to be a neutron star in the supernova remnant N49 in the Large Magellanic Cloud. In this model, the observed radiation is produced in the skin layer of a hot, radiation-dominated pair atmosphere, probably confined to the vicinity of the neutron star by a strong magnetic field. In this layer, about 10 to the 12th generations of pairs are formed (by photon-photon collisions), cooled and annihilated during the 0.15 s duration of the impulsive phase.

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