• DOI:10.1134/S0038094606040046
• Corpus ID: 121291767

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

@article{Grechnev2006LonglivedHC,
  title={Long-lived hot coronal structures observed with CORONAS-F/SPIRIT in the Mg XII line},
  author={V. V. Grechnev and Sergey V. Kuzin and A. M. Urnov and Igor A. Zhitnik and Arkadiy M. Uralov and S. A. Bogachev and Moissei Livshits and O. I. Bugaenko and Vasiliy G. Zandanov and A. P. Ignat’ev and Viktor V. Krutov and S. N. Oparin and Andrei A. Pertsov and Vladimir Slemzin and I. M. Chertok and Alexandr I. Stepanov},
  journal={Solar System Research},
  year={2006},
  volume={40},
  pages={286-293}
}

• V. Grechnev, S. Kuzin, +13 authors A. Stepanov
• Published 1 July 2006
• Physics
• Solar System Research

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, Tmax = 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 1 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 ne ≈ 1010 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 β ≪ 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.”