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Wave Activity and Prominence Eruption

Published online by Cambridge University Press:  12 April 2016

F. Baudin ,
K. Bocchialini ,
C. Delannee ,
S. Koutchmy ,
G. Stellmacher ,
K. Shibata ,
I.S. Veselovsky ,
O.A. Panasenko  and
A.N. Zhukov
F. Baudin
Affiliation:
Institut d’Astrophysique Spatiale/Univ. Paris XI Bât. 121, Campus d’Orsay, 91405 Orsay, France
K. Bocchialini
Affiliation:
Institut d’Astrophysique Spatiale/Univ. Paris XI Bât. 121, Campus d’Orsay, 91405 Orsay, France
C. Delannee
Affiliation:
Institut d’Astrophysique de Paris/CNRS, 98 Bis Bd Arago, 75014 Paris, France
S. Koutchmy
Affiliation:
Institut d’Astrophysique de Paris/CNRS, 98 Bis Bd Arago, 75014 Paris, France
G. Stellmacher
Affiliation:
Institut d’Astrophysique de Paris/CNRS, 98 Bis Bd Arago, 75014 Paris, France
K. Shibata
Affiliation:
National Astronomical Observatory, Mitaka 181 Tokyo, Japan
I.S. Veselovsky
Affiliation:
Institute of Nuclear Physics, Moscow State University, Moscow 119899, Russia
O.A. Panasenko
Affiliation:
Institute of Nuclear Physics, Moscow State University, Moscow 119899, Russia
A.N. Zhukov
Affiliation:
Institute of Nuclear Physics, Moscow State University, Moscow 119899, Russia

Abstract

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Observational evidence of 3 and 5 min vertical oscillations of a filament on the disk are recorded. Wave activity was observed before, during and after a filament disappearance, inside and around the filament. Both an Hα brightening and, later, a blowing out of a faint soft X-ray (Yohkoh) loop system occuring in connection with a flare were noticed. The wave activity seems to be a dynamically important ingredient of this erupting prominence.

Propagating MHD waves and convective structures bring their energy and momentum from the photosphere towards the chromosphere up to the coronal heights where they are partially reflected and/or dissipated. The transition from the laminar to the turbulent state of the whole prominence enhances the dissipation rate of the external waves inside this system, adding energy to produce the heating and lifting of the plasma. Internal plasma instabilities could trigger this transition in the framework of a prominence disappearance.

Type
Birth and Death of Filaments
Information
International Astronomical Union Colloquium , Volume 167: New Perspectives on Solar Prominences , 1998 , pp. 314 - 317
Copyright
Copyright © Astronomical Society of the Pacific 1998

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