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The exceptional aspects of the confined X-class flares of solar active region 2192

Published online by Cambridge University Press:  09 September 2016

Julia K. Thalmann ,
Yang Su ,
Manuela Temmer  and
Astrid M. Veronig
Julia K. Thalmann
Affiliation:
Institute of Physics/IGAM, University of Graz, Universittsplatz 5/II, 8010 Graz, Austria email: [email protected]
Yang Su
Affiliation:
Institute of Physics/IGAM, University of Graz, Universittsplatz 5/II, 8010 Graz, Austria email: [email protected] Key Laboratory of Dark Matter & Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, 2 West Beijing Road, 210008 Nanjing, China email: [email protected]
Manuela Temmer
Affiliation:
Institute of Physics/IGAM, University of Graz, Universittsplatz 5/II, 8010 Graz, Austria email: [email protected]
Astrid M. Veronig
Affiliation:
Institute of Physics/IGAM, University of Graz, Universittsplatz 5/II, 8010 Graz, Austria email: [email protected]
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Abstract

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During late October 2014, active region NOAA 2192 caused an unusual high level of solar activity, within an otherwise weak solar cycle. While crossing the solar disk, during a period of 11 days, it was the source of 114 flares of GOES class C1.0 and larger, including 29 M- and 6 X-flares. Surprisingly, none of the major flares (GOES class M5.0 and larger) was accompanied by a coronal mass ejection, contrary to statistical tendencies found in the past. From modeling the coronal magnetic field of NOAA 2192 and its surrounding, we suspect that the cause of the confined character of the flares is the strong surrounding and overlying large-scale magnetic field. Furthermore, we find evidence for multiple magnetic reconnection processes within a single flare, during which electrons were accelerated to unusual high energies.

Keywords

Sun: atmosphereSun: chromosphereSun: coronaSun: magnetic fieldsSun: flaresSun: UV radiationSun: X-raysgamma raysmethods: numerical
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S320: Solar and Stellar Flares and their Effects on Planets , August 2015 , pp. 60 - 63
Copyright
Copyright © International Astronomical Union 2016 

References

Pötzi, W., Veronig, A. M., Riegler, G., Amerstorfer, U., Pock, T., Temmer, M., Polanec, W., & Baumgartner, D. J. 2015, Sol. Phys., 290, 951 Google Scholar
Sun, X., Bobra, M. G., Hoeksema, J. T., Liu, Y., Li, Y., Shen, C., Couvidat, S., Norton, A. A., & Fisher, G. H. 2015, ApJ (Letters), 804, L28 Google Scholar
Thalmann, J. K., Su, Y., Temmer, M., & Veronig, A. M. 2015, ApJ (Letters), 801, L23 Google Scholar
Török, T. & Kliem, B. 2005, ApJ (Letters), 630, L97 Google Scholar
Kliem, B. & Török, T. 2006, Phys. Rev. (Letters), 96, 255002 Google Scholar
Veronig, A. M. & Polanec, W. 2015, Sol. Phys., 290, 2923 Google Scholar
Wang, Y. & Zhang, J. 2007, ApJ, 665, 1428 Google Scholar
Yashiro, S., Akiyama, S., Gopalswamy, N., & Howard, R. A. 2006, ApJ (Letters), 650, L143 Google Scholar