Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://www.sao.ru/cats/~satr/RFSymp/abs/04_Borovik.ps Äàòà èçìåíåíèÿ: Mon Oct 9 11:14:23 2006 Äàòà èíäåêñèðîâàíèÿ: Tue Oct 2 08:56:44 2012 Êîäèðîâêà: Ïîèñêîâûå ñëîâà: m 80

MULTIWAVE RATAN­600 OBSERVATIONS OF
POST­ERUPTIVE PROCESSES ON THE SUN
V.N. Borovik 1 , V.V. Grechnev 2 , V.E. Abramov­Maksimov 1 , I.Y. Grigorieva 1 , V.M.
Bogod 3 , V.I. Garaimov 3 , T.I. Kaltman 3 , A.N. Korzhavin 3
1 Central Astronomical Observatory of RAS, Saint­Petrsburg, Pulkovskoje shosse, 65,
2 Institute of Solar Terrestrial Physics, Irkutsk,
3 Special Astrophysical Observatory of RAS, Saint­Petrsburg, Pulkovskoe schosse, 65,
Russia
borovik@saoran.spb.su
During two last decades, authors of some studies of post­eruptive arcades repeatedly came
to the following unexpected conclusions. Microwave emission of arcades was excessively
polarized, presumably due to contribution of non­thermal electrons. Their lifetime was
much longer than the estimated cooling times, presumably due to the post­eruptive energy
release. Finally, the plasma pressure exceeded the magnetic pressure (# # 1) in their
hot top parts. CORONAS­F/SPIRIT observations in the high­temperature (#10 MK)
line MgXII and multi­wave RATAN­600 observations along with data from other spectral
domains provided important information to verify these conclusions and assumptions. All
above facts were confirmed in analyses of this data set. They were explained in terms
of the standard flare model (``CSHKP'') elaborated by Yokoyama & Shibata (1998) to
qualitative account for the chromospheric evaporation, but applied to late post­eruptive
phase. In this case, high # conditions indicate magnetic reconnection processes responsible
for the prolonged heating and particle acceleration. This approach allows to reconcile the
listed facts with known estimates of parameters of the coronal plasma in post­eruptive
arcades, and to remove seeming contradictions with habitual conceptions. We consider
long­lived post­eruptive arcades observed on 22 October 2001, 2 November 1992, and 28--
30 December 2001 and demonstrate that these conclusions are valid, because high­density
hot regions in their top parts (thus, high # regions) existed for a long time, and their
radio emission contained non­thermal component, which is indicative of the presence of
accelerated particles.
References
Yokoyama T., Shibata K.: 1998, ApJ, 494, L113.