Spectral evolution of the 5 March 1979 gamma burst

Details Spectral evolution of the 5 March 1979 gamma burst Spectral evolution of the 5 March 1979 gamma burst

Jan 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981natur.289...42f&link_type=abstract

Nature, vol. 289, Jan. 8, 1981, p. 42, 43. Research supported by the U.S. Department of Energy and NASA.

Astronomy and Astrophysics

Astronomy

15

Gamma Ray Spectra, Neutron Stars, Pulsars, Pulsed Radiation, Spaceborne Astronomy, Bursts, Gamma Ray Astronomy, Pioneer Venus 1 Spacecraft, Stellar Magnetic Fields, Stellar Rotation

Scientific paper

The spectral development of the intense gamma-ray burst observed on March 5, 1979 by nine spacecraft spaced on an interplanetary scale is discussed. As observed by the Pioneer Venus Orbiter detector, the hardness ratio of the burst, defined as the ratio between counts in the 100-1000 keV channels to those in the 50-100 keV channel, decreases during the very fast rise and subsequent 75 msec of the burst, consistent with a decrease in black-body temperature from 30 to 26 keV, and then increases during the shoulder on the gamma-ray burst light curve. Following the burst, the source was observed to exhibit many of the characteristics of a hard X-ray pulsar with a period of 8.0 sec and a hardness ratio varying in phase with the intensity. The observed characteristics of the pulsations are interpreted in terms of hot spots at the magnetic poles of a rotating neutron star, although it is shown that the simple cooling of residual hot spots does not completely explain the pulsations. Alternative explanations for the pulsation include accretion or an effect of beam geometry.

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