NDLI: Solar proton flare 4B/X17.2 on October 28, 2003. Photometric results

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Kinematics and Physics of Celestial Bodies : Volume 33

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Some results of investigating the stability of operation of the Ukrainian laser ranging stations

Modeling the changes of physical parameters of the atmosphere with height

Synchrotron and thermal X-ray emission from supernova remnants. Low radiation losses of electrons

Energy of solar noise-storm radio bursts

Solar proton flare 4B/X17.2 on October 28, 2003. Photometric results

Chromospheric telescope modification for digital imaging

Solar proton flare 4B/X17.2 on October 28, 2003. Photometric results

Content Provider	Springer Nature Link
Author	Laba, I. S.
Copyright Year	2007
Abstract	The powerful flare 4B/X17.2 of October 28, 2003 in the NOAA 10486 active region is studied by using H$_{α}$ filtergrams. This active region had a complicated βγδ magnetic configuration and a sigmoidal pattern of the polarity inversion line, it had the largest AR area in the cycle 23. Local filaments, loops, and systems of loops were also observed in the AR. The light curves obtained for all flare knots clearly reveal two stages in their evolution. The first stage is the pre-flare one, when the accumulation of the nonpotential magnetic energy (the energy of electric currents) comes to an end and the situation becomes favorable for the realization of the second period. The intensity of flare knots (except one knot) changed slightly and slowly, and some structure features (twists and connections) became more active. By the end of the first stage a new magnetic flux emerged and a system of interrelated filaments and loops (IFL) was formed at the center of the AR as well as at its periphery. New flare knots appeared about the main S-like filament. The second flare stage began at about 11:02 UT with a dramatic increase of the intensity and area of all flare knots and the formation of new knots. In a space of 8 min the major part of the AR around the main filament was covered with flare emission which fluctuated at its maximum period. The intensity of all knots was observed to drop slowly after the maximum, at the decay phase. As the IFL system extended over the entire AR, the magnetic field energy accumulated in it was released in the form of powerful electromagnetic and corpuscular emission by way of magnetic reconnection.
Starting Page	36
Ending Page	40
Page Count	5
File Format	PDF
ISSN	08845913
Journal	Kinematics and Physics of Celestial Bodies
Volume Number	23
Issue Number	1
e-ISSN	19348401
Language	English
Publisher	Allerton Press, Inc.
Publisher Date	2007-01-01
Publisher Place	New York
Access Restriction	One Nation One Subscription (ONOS)
Subject Keyword	Astronomy
Content Type	Text
Resource Type	Article
Subject	Astronomy and Astrophysics Space and Planetary Science

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