Giant flare in SGR 1806-20 and its Compton reflection from the Moon

被引：60

作者：

Frederiks, D. D.

Golenetskii, S. V.

Palshin, V. D.

Aptekar, R. L.

Ilyinskii, V. N.

Oleinik, F. P.

Mazets, E. P.

Cline, T. L.

机构：

[1] Russian Acad Sci, AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia

[2] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

来源：

ASTRONOMY LETTERS-A JOURNAL OF ASTRONOMY AND SPACE ASTROPHYSICS | 2007年 / 33卷 / 01期

基金：

俄罗斯基础研究基金会;

关键词：

neutron stars; flares; gamma rays; Compton scattering;

D O I：

10.1134/S106377370701001X

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We analyze the data obtained when the Konus-Wind gamma-ray spectrometer detected a giant flare in SGR 1806-20 on December 27, 2004. The flare is similar in appearance to the two known flares in SGR 0526-66 and SGR 1900+14 while exceeding them significantly in intensity. The enormous X-ray and gamma-ray flux in the narrow initial pulse of the flare leads to almost instantaneous deep saturation of the gamma-ray detectors, ruling out the possibility of directly measuring the intensity, time profile, and energy spectrum of the initial pulse. In this situation, the detection of an attenuated signal of inverse Compton scattering of the initial pulse emission by the Moon with the Helicon gamma-ray spectrometer onboard the Coronas-F satellite was an extremely favorable circumstance. Analysis of this signal has yielded the most reliable temporal, energy, and spectral characteristics of the pulse. The temporal and spectral characteristics of the pulsating flare tail have been determined from Konus-Wind data. Its soft spectra have been found to contain also a hard power-law component extending to 10 MeV. A weak afterglow of SGR 1806-20 decaying over several hours is traceable up to 1 MeV. We also consider the overall picture of activity of SGR 1806-20 in the emission of recurrent bursts before and after the giant flare.

引用

页码：1 / 18

页数：18

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