Peculiarities of X-ray emission of the solar flare on 29 October 2002

P. B. Dmitriev1, I. V. Kudryavtsev1,2, V. P. Lazutkov1, G. A. Matveev1, M. I. Savchenko1, and D. V. Skorodumov1

1A. F. Ioffe Physical and Technical Institute, Russian Academy of Sciences, St. Petersburg, Russia
2Central Astronomical Observatory at Pulkovo, Russian Academy of Sciences, St. Petersburg, Russia


[1]  Time structure of the soft and hard X-ray emission of the solar flare on 29 October 2002 is studied. The flare began at 2148:49 UT and was measured by the IRIS spectrometer on board the CORONAS-F spacecraft. High sensitivity of the device made it possible to detect in the flare X-ray emission a pulse structure with timescale of the order of tens of milliseconds. Similarly, spike structure was observed on board of Compton Gamma Ray Observatory. A quasiperiodic structure with a magnitude of the order of 10 s was revealed by means of spectral time analysis. This structure can be explained by magnetohydrodynamic sausage-mode oscillations generated in the flare loop with the characteristic parameters of the plasma of the coronal region of the solar atmosphere. The evolution of the energetic spectrum of the hard X-ray emission of this flare with the resolution of 1 s during the entire event is studied.

Received 20 January 2006; accepted 12 February 2007; published 11 May 2007.

Keywords: X-ray emission; Solar flares; CORONAS-F.

Index Terms: 2164 Interplanetary Physics: Solar wind plasma; 7519 Solar Physics, Astrophysics, and Astronomy: Flares; 2199 Interplanetary Physics: General or miscellaneous.


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