Gamma-ray bursts from young neutron stars

Details Gamma-ray bursts from young neutron stars Gamma-ray bursts from young neutron stars

Jan 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982aipc...77..293b&link_type=abstract

In: Gamma ray transients and related astrophysical phenomena; Proceedings of the Workshop, La Jolla, CA, August 5-8, 1981. (A83-

Astronomy and Astrophysics

Astronomy

5

Gamma Ray Bursts, Neutron Stars, Pulsars, Stellar Radiation, Supernova Remnants, Crab Nebula, Gamma Ray Astronomy, Magellanic Clouds, Orbital Elements, Stellar Evolution, Stellar Rotation

Scientific paper

Data from the Mar. 5, 1979 gamma ray burst (M5) from the supernova remnant N49 are used to examine the nature of gamma ray burst sources. The association with N49 was statistically linked at the 0.04% level, thus ruling out a superposition phenomenon. The burst was calculated to be emitted from a source with a 10 to the 44th erg/sec peak luminosity, and displayed an 8.1 sec periodicity, which is taken as the free precession period of a rotating neutron star. The rotation interval is suggested to be from 10-100 msec. A connection between the gamma ray events and pulsar glitches, e.g., an abrupt change in the pulsar period, is explored. A 0.001 erg/sq cm pulse is predicted to be emitted from such an event, much smaller than the M5 levels. The possibility that superglitches occur as a result of transitions between interior equilibriums in neutron stars is discussed. Finally, a connection between the gamma ray bursts and young neutron stars is proposed, with bursts being the result of a postformation glitch, phase transition, or other stellar activity. Observational techniques for validating the model are outlined.

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