Long-lived hot coronal structures observed with CORONAS-F/SPIRIT in the Mg XII line

被引:19
作者
Grechnev, V. V.
Kuzin, S. V.
Urnov, A. M.
Zhitnik, I. A.
Uralov, A. M.
Bogachev, S. A.
Livshits, M. A.
Bugaenko, O. I.
Zandanov, V. G.
Ignat'ev, A. P.
Krutov, V. V.
Oparin, S. N.
Pertsov, A. A.
Slemzin, V. A.
Chertok, I. M.
Stepanov, A. I.
机构
[1] Russian Acad Sci, Siberian Branch, Inst Solar Terr Phys, Irkutsk 664033, Russia
[2] Russian Acad Sci, PN Lebedev Phys Inst, Moscow 117924, Russia
[3] Russian Acad Sci, Pushkov Inst Terr Magnetism Ionosphere & Radio Wa, Troitsk 142090, Moscow Region, Russia
[4] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119899, Russia
基金
俄罗斯基础研究基金会;
关键词
D O I
10.1134/S0038094606040046
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Large-scale hot features were detected and observed several times high in the solar corona in the high-temperature Mg XII line (T = 5-20 MK, T-max = 10 MK) with the soft X-ray telescope of the SPIRIT instrumentation complex onboard the CORONAS-F spacecraft. These features look like a spider up to 300000 km in size and live up to a few days. Their bright cores observed at heights were from 0.1 to 0.3 solar radii are connected with active regions by darker legs, giant loops. These features are disposed above arcades, which are simultaneously observed in cooler emission lines sensitive to temperatures of I to 2 MK. For the core of such a feature observed December 28-29, 2001, Zhitnik et al. (2003a) estimated an electron temperature of 10 MK and a number density of n(e) approximate to 10(10) cm(-3). A high activity and an association with eruptive phenomena were found for such features in continuous (up to 20-day) observations with a cadence of 0.6-1.7 min. In the present paper, we discuss the relation of such features to coronal structures, which are known from previous studies. We identify such off-limb features observed with SPIRIT on October 22, November 12, and December 28-29, 2001, with hot upper parts of post-eruptive arcades. The results of multifrequency analysis of these features based on the data obtained in various spectral ranges by different instruments (Yohkoh/SXT, SOHO/EIT, SOHO/LASCO, Nobeyama and SSRT radioheliographs) are briefly discussed. We address the physical conditions of the long-term existence of giant hot coronal structures. It is demonstrated that the post-eruptive energy release must be prolonged and the condition beta << 1 is not satisfied in these structures. It is argued that the so-called "standard flare model" should be better considered as a "standard post-eruptive energy release model."
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收藏
页码:286 / 293
页数:8
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