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MULTIWAVE RATAN-600 OBSERVATIONS OF POST-ERUPTIVE PROCESSES ON THE SUN
V.N. Borovik1 , V.V. Grechnev2 , V.E. Abramov-Maksimov1 , I.Y. Grigorieva1 , V.M. Bogo d3 , V.I. Garaimov3 , T.I. Kaltman3 , A.N. Korzhavin3
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Central Astronomical Observatory of RAS, Saint-Petrsburg, Pulkovsko je shosse, 65, 2 Institute of Solar Terrestrial Physics, Irkutsk, Sp ecial Astrophysical Observatory of RAS, Saint-Petrsburg, Pulkovsko e schosse, 65, Russia b orovik@saoran.spb.su

During two last decades, authors of some studies of p ost-eruptive arcades rep eatedly came to the following unexp ected conclusions. Microwave emission of arcades was excessively p olarized, presumably due to contribution of non-thermal electrons. Their lifetime was much longer than the estimated co oling times, presumably due to the p ost-eruptive energy release. Finally, the plasma pressure exceeded the magnetic pressure ( 1) in their hot top parts. CORONAS-F/SPIRIT observations in the high-temp erature (10 MK) line MgXI I and multi-wave RATAN-600 observations along with data from other sp ectral domains provided imp ortant information to verify these conclusions and assumptions. All ab ove facts were confirmed in analyses of this data set. They were explained in terms of the standard flare mo del ("CSHKP") elab orated by Yokoyama & Shibata (1998) to qualitative account for the chromospheric evap oration, but applied to late p ost-eruptive phase. In this case, high conditions indicate magnetic reconnection pro cesses resp onsible 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 p ost-eruptive arcades, and to remove seeming contradictions with habitual conceptions. We consider long-lived p ost-eruptive arcades observed on 22 Octob er 2001, 2 Novemb er 1992, and 28­ 30 Decemb er 2001 and demonstrate that these conclusions are valid, b ecause high-density hot regions in their top parts (thus, high regions) existed for a long time, and their radio emission contained non-thermal comp onent, which is indicative of the presence of accelerated particles. References Yokoyama T., Shibata K.: 1998, ApJ, 494, L113.