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Magnetic Field Reconnection in the Hα Eruptive Prominence on September 18, 1995

Published online by Cambridge University Press:  12 April 2016

Marian Karlický ,
Pavel Kotrč ,
Stanislava Šimberová ,
Miloslav Knížek  and
Michal Varady
Marian Karlický
Affiliation:
Astronomical Institute of the Academy of Sciences of Czech Republic, CZ-251 65 Ondřejov, Czech Republic
Pavel Kotrč
Affiliation:
Astronomical Institute of the Academy of Sciences of Czech Republic, CZ-251 65 Ondřejov, Czech Republic
Stanislava Šimberová
Affiliation:
Astronomical Institute of the Academy of Sciences of Czech Republic, CZ-251 65 Ondřejov, Czech Republic
Miloslav Knížek
Affiliation:
Astronomical Institute of the Academy of Sciences of Czech Republic, CZ-251 65 Ondřejov, Czech Republic
Michal Varady
Affiliation:
Astronomical Institute of the Academy of Sciences of Czech Republic, CZ-251 65 Ondřejov, Czech Republic

Abstract

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A violent evolution of the September 18, 1995 eruptive prominence is studied. The fast changes of the prominence structure started immediately after a weak radio burst on 3 GHz indicating the presence of non-thermal processes. A comparison with Yohkoh soft X-ray pictures was made. A detailed analysis of observations indicates magnetic field line reconnection, mainly in the space below the rising Hα prominence. The reconnection processes are manifested by structural changes of the Hα prominence and X-ray loops and also by the character of Doppler velocities in the Hα spectrum formed close to the reconnection space.

Type
Birth and Death of Filaments
Information
International Astronomical Union Colloquium , Volume 167: New Perspectives on Solar Prominences , 1998 , pp. 310 - 313
Copyright
Copyright © Astronomical Society of the Pacific 1998

References

Kotr, P., Heinzel, P. and Knek, M. 1993, in JOSO Annual Report 1992, (ed.) Alvensleben, A.v., Freiburg, p. 114 Google Scholar
Pevtsov, A.A., Canfield, R.C. and Zirin, H. 1996, ApJ, 473, 533 Google Scholar
Rompolt, B. 1990, Hvar Obs. Bull., 14, 37 Google Scholar
Sakai, J. (ed.) 1993, Proceedings of Symposium on Current Loop Interaction in Solar Flares, Toyama University Google Scholar
Smartt, R.N., Zhang, Z., Kim, I.S. and Reardon, K.P. 1994, in Solar Coronal Structures, Rušin, V. et al. (eds.), VEDA Publ. Co., Bratislava, p. 219 Google Scholar
Šimberová, S., Karlický, M. and Švestka, Z. 1993, Solar Phys., 146, 343 Google Scholar
Švestka, Z. and Cliver, E.W. 1992, in Eruptive Solar Flares, (eds.) Švestka, Z., Jackson, B. and Machado, M., Springer-Verlag, Berlin, p. 1 Google Scholar
Tandberg-Hanssen, E. 1995, The Nature of Solar Prominences, Kluwer Acad. Publ., Dordrecht, Holland Google Scholar
Tsuneta, S. 1996, ApJ, 456, L63 Google Scholar