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Different Stages of Evolution of Prominence and the Associated CMEs

Published online by Cambridge University Press:  06 January 2014

Lela Taliashvili ,
Zadig Mouradian  and
Heidy Gutiérrez
Lela Taliashvili
Affiliation:
Space Research Center, University of Costa Rica, 2060 San Jos, Costa Rica email: lela.taliashvili@cinespa.ucr.ac.cr
Zadig Mouradian
Affiliation:
Observatoire de Paris–Meudon, LESIA, 92190 Meudon, France
Heidy Gutiérrez
Affiliation:
Space Research Center, University of Costa Rica, 2060 San Jos, Costa Rica email: lela.taliashvili@cinespa.ucr.ac.cr
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Abstract

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We study the different evolutional stages of a large quiescent prominence, mainly considering its dynamic/thermal instabilities occurred close from the boundary of coronal hole (CH). We identify the critical conditions, such as the minimum distance between the CH's boundary and prominence channel and the emergence of a new magnetic flux linked to the prominence instability and its general evolution in connection to CH. Our observations indicate peculiar filament activations prior to its thermal/dynamic instabilities, suggesting the connection of nearby CH with the general evolution of prominence and vice versa. Additionally, we analyze each evolutional stage of prominence and the associated Coronal Mass Ejections (CMEs).

Keywords

Prominencecoronal holecoronal mass ejectionmagnetic fluxmagnetic field
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S300: Nature of Prominences and their role in Space Weather , June 2013 , pp. 497 - 499
Copyright
Copyright © International Astronomical Union 2013 

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