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Distinguishing between coronal cloud prominences and channel prominences and their associations with solar and stellar flares

Published online by Cambridge University Press:  09 September 2016

Sara F. Martin ,
Oddbjorn Engvold ,
Yong Lin  and
Jacqueline Alves da Silva
Sara F. Martin
Affiliation:
Helio Research, 5212 Maryland Ave., La Crescenta, CA 91214, USA email: sara@helioresearch.org
Oddbjorn Engvold
Affiliation:
Institute of Theoretical Astrophysics, University of Oslo, P.O. Box 1029, Blindern, 0315 Oslo, Norway email: oddbjorn.engvold@astro.uio.no
Yong Lin
Affiliation:
Geodetic Institute, Norwegian Mapping Authority, Kartverksveien 21, 3511 Honefoss, Norway email: angeline_lin@hotmail.com
Jacqueline Alves da Silva
Affiliation:
Florida Institute of Technology, Melbourne, FL, USA email: jalvesdasilv2015@my.fit.edu
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Abstract

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To better understand the differences between coronal cloud prominences and channel prominences, we systematically identified and analyzed coronal cloud prominences recorded in SDO/AIA images at 304 Å from 2010 May 20 through 2012 April 28. For the 225 cases identified, their numbers vary directly with the sunspot number. Their durations are typically less than 3 days. Their most frequent maximum height is 90,000 + and - 10,000 km. We offer our hypothesis that many coronal cloud prominences originate from some of the mass of previously erupted filaments ejected high out of their filament channels; subsequently part of this mass falls and collects in leaky magnetic troughs among coronal magnetic fields which constrain the leaked mass to slowly drain downward along curved trajectories where it appears as coronal rain. Currently there is inadequate evidence for a convincing correspondence between either coronal cloud prominences or channel prominences with stellar prominences detected to date.

Keywords

prominencesfilamentscorona
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. 278 - 287
Copyright
Copyright © International Astronomical Union 2016 

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