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Observations of the Association of Prominences and the Surrounding Corona

Published online by Cambridge University Press:  12 April 2016

Raymond N. Smartt ,
Zhenda Zhang ,
Vladimir S. Airapetian  and
Ira S. Kim
Raymond N. Smartt
Affiliation:
National Solar Observatory/Sacramento Peak, National Optical Astronomical Observatories, P.O. Box 62, Sunspot, NM 88349, USA
Zhenda Zhang
Affiliation:
Department of Astronomy, Nanjing University, Nanjing, China
Vladimir S. Airapetian
Affiliation:
Code 681/CSC, NASA/GSFC, Greenbelt, MB 20771, USA
Ira S. Kim
Affiliation:
Sternberg State Astronomical Institute, Moscow State University, Universitetsky pr. 13, 119899 Moscow, Russia

Abstract

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Emission-line coronal images in Fe XIV (530.3 nm) and FeX (637.5 nm) show faint enhancements at the location of quiescent prominences. Such enhancements can appear in the outer portions of a prominence, similar to the high-temperature sheath surrounding prominences as inferred from UV and EUV observations. The observational evidence supports the interpretation that this enhanced coronal emission is due to energy carried by the prominence threads and dissipated in the adjacent coronal region. Also, observed coronal loop interactions involving partial magnetic reconnection have associated Hα structures. These structures can have the appearance of an active prominence, similar to those typically observed in post flare loop systems. It appears that the association of such active prominences with the adjacent corona is fundamentally different from that of quiescent prominences. The observations indicate that these types of active prominences arise simply as a consequence of reconnection processes in the corona itself.

Type
Filaments and Their Environment
Information
International Astronomical Union Colloquium , Volume 167: New Perspectives on Solar Prominences , 1998 , pp. 37 - 40
Copyright
Copyright © Astronomical Society of the Pacific 1998

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