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November 4, 2001  

Solar Eruptive Event of 4 November 2001 observed with the SPIRIT Telescope on Board the CORONAS-F Satellite

I. M. Chertok(1),  V. A. Slemzin(2), S. V. Kuzin(2), V. V. Grechnev(3), O. I. Bugaenko(4), I. A. Zhitnik(2), A. P. Ignatiev(2), A. A. Pertsov(2)

(1) IZMIRAN, Troitsk, Moscow Region, 142190, Russia
(2) P.N.Lebedev Physics Institute of RAS, Moscow, 117924, Russia
(3) ISTP SD RAS, Irkutsk, 664033, Russia
(4) Sternberg Astronomical Institute, Moscow University, Moscow, 119899, Russia

Based on the data of the SPIRIT telescope on board the CORONAS-F satellite in three EUV channels 175, 284, 304 Å, we have analyzed large-scale manifestations of the post-eruptive so-lar activity followed one of the most considerable and geoeffective coronal mass ejection (CME) in the 23rd cycle which occurred on 4 November 2001. In particular, we have shown that the re-configuration of the magnetic field over the eruptive center was accompanied by a formation of a multi-component post-eruptive arcade extending over about 0.5 Rs that was observed in all three SPIRIT channels during many hours. Both compact and channeled dimmings were observed on each side of this arcade and also along some extended structures outside the active region, rescpectively. The emission intensity in those dimmings was suppressed by tens percent. The observed enhanced emission at the upper part of the posteruptive arcade can be caused by energy release which took place high in the corona due to the process of magnetic reconnection during the relaxation stage of the magnetic field disturbed by a CME to a new equilibrium closed con-figuration. Another possible reason of this effect is an excess of the emission measure due to the passage of the line of sight simultaneously along the upper part and basis of the posteruptive loops observed on the angle. The spatial coincidence of the main dimmings in the diverse-temperature lines denotes their origin as a result of the plasma evacuation from transition-region and coronal structures with open field lines. For some dimmings whose appearance differs in dif-ferent lines, CME-associated variations of the plasma temperature are important as well.

16:20 UT, 3B/X1.0, AR 9684 (N06 W18), halo CME,
GLE, J(>10 MeV)~3000 p.f.u., Dst~-300 nT

Situation before the event ;   GOES soft X-rays and CME ;

H-alpha flare, Holloman Observatory

Halo CME observed with SOHO/LASCO  ;

Posteruptive arcade on the CORONAS-F/SPIRIT movies at
                    175 Å ,  284 Å , 304 Å

Yohkoh/SXT movie

Posteruptive arcade by the CORONAS-F/SPIRIT data at 175, 284, 304 Å and by the Yohkoh/SXT data ;

Dimmings on the CORONAS-F/SPIRIT rerotated fixed difference images at at 175, 284, 304 Å ;

Dimmings on the CORONAS-F/SPIRIT movies at
                    175 Å ,  284 Å , 304 Å
 

Comparison with the Bastille Day Event of July 14, 2000:

     Solar Manifestations ;   Posteruptive arcade with a spine ;

    Space Weather Phenomena ;

 PDF file and Figures  1 ,  2 ,  3 ,  4 of the paper "Solar Eruptive Event of 4 November 2001 observed with the SPIRIT Telescope on Board the CORONAS-F Satellite", by I. M. Chertok,  V. A. Slemzin, S. V. Kuzin, V. V. Grechnev, O. I. Bugaenko, I. A. Zhitnik, A. P. Ignatiev, A. A. Pertsov,  Astronomicheskii Zhurnal (in Russian), Vol. 81, No. 5, pp. 447-458, 2004.

PDF file of the English translation of the the paper:  Astronomy Reports, Vol. 48, No. 5, pp. 407-417, 2004.

        See the  CORONAS-F/SPIRIT site


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