The Konus-Wind and Helicon-Coronas-F detection of the giant $γ$-ray flare from the soft $γ$-ray repeater SGR 1806-20

Details The Konus-Wind and Helicon-Coronas-F detection of the giant $γ$-ray flare from the soft $γ$-ray repeater SGR 1806-20 The Konus-Wind and Helicon-Coronas-F detection of the giant $γ$-ray flare from the soft $γ$-ray repeater SGR 1806-20

2005-02-25

arxiv.org/abs/astro-ph/0502541v1

Astronomy and Astrophysics

Astrophysics

5 pages, 7 figures

Scientific paper

The giant outburst from SGR 1806-20 was observed on 2004 December 27 by many spacecraft. This extremely rare event exhibits a striking similarity to the two giant outbursts thus far observed, on 1979 March 5 from SGR 0526-66 and 1998 August 27 from SGR 1900+14. All the three outbursts start with a short giant radiation pulse followed by a weaker tail. The tail pulsates with the period of neutron star rotation of $\sim$5--8 s, to decay finally in a few minutes. The enormous intensity of the initial pulse proved to be far above the saturation level of the gamma-ray detectors, with the result that the most valuable data on the time structure and energy spectrum of the pulse is lost. At the time of the December 27 outburst, a Russian spacecraft Coronas-F with a $\gamma$-ray spectrometer aboard was occulted by the Earth and could not see the outburst. It succeeded, however, in observing a weak reflected signal due to the $\gamma$-rays Compton scattered by the Moon. This has been the first observation of a cosmic gamma-ray flare reflected from a celestial body. Here we report, that the detection of a weakened back-scattered initial pulse combined with direct observations by the Konus $\gamma$-ray spectrometer on the Wind spacecraft permitted us to reliably reconstruct the intensity, time history, and energy spectra of the outburst.

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