A giant periodic flare from the soft γ-ray repeater SGR1900+14

K. Hurley (), T. Cline, E. Mazets, S. Barthelmy, P. Butterworth, F. Marshall, D. Palmer, R. Aptekar, S. Golenetskii, V. Il'Inskii, D. Frederiks, J. McTiernan, R. Gold and J. Trombka
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K. Hurley: UC Berkeley Space Sciences Laboratory
T. Cline: NASA Goddard Space Flight Center
E. Mazets: Ioffe Physical-Technical Institute
S. Barthelmy: NASA Goddard Space Flight Center
P. Butterworth: NASA Goddard Space Flight Center
F. Marshall: Ioffe Physical-Technical Institute
D. Palmer: NASA Goddard Space Flight Center
R. Aptekar: Ioffe Physical-Technical Institute
S. Golenetskii: Ioffe Physical-Technical Institute
V. Il'Inskii: Ioffe Physical-Technical Institute
D. Frederiks: Ioffe Physical-Technical Institute
J. McTiernan: UC Berkeley Space Sciences Laboratory
R. Gold: The Johns Hopkins University, Applied Physics Laboratory
J. Trombka: NASA Goddard Space Flight Center

Nature, 1999, vol. 397, issue 6714, 41-43

Abstract: Abstract Soft γ-ray repeaters are transient sources of high-energy photons; they emit sporadic and short (about 0.1 s) bursts of ‘soft’ γ-rays during periods of activity, which are often broken by long stretches of quiescence. These objects are associated with neutron stars in young supernova remnants1. The event of 5 March 1979 was the most intense burst to date, and the only one that showed a clear periodicity in the signal2,3. Here we report the detection, on 27 August 1998, of an even more intense burst from a different soft γ-ray repeater. This event was characterized by ‘hard’ γ-rays at its peak, followed by a tail 300 s long with a soft spectrum and a clear periodicity of 5.16 s. The burst was probably initiated by a massive disruption of the crust of the neutron star, followed by an outflow of energetic particles rotating with the period of the star. A comparison of the events of 27 August 1998 and 5 March 1979 supports the idea that magnetic energy plays an important role in the genesis of such events. Although these giant flares are rare, they are not unique events and may occur at any time in a neutron star's activity cycle.

Date: 1999
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DOI: 10.1038/16199

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