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Understanding structures at the base of the solar corona – polar plumes

Published online by Cambridge University Press:  01 September 2008

A. H. Gabriel ,
F. Bely-Dubau ,
E. Tison  and
L. Abbo
A. H. Gabriel
Affiliation:
Institut d'Astrophysique Spatial, Université Paris Sud-11, 91405 Orsay Cedex, France email: gabriel@ias.fr
F. Bely-Dubau
Affiliation:
Observatoire de la Côte d'Azur, BP4229, 06304 Nice Cedex, France
E. Tison
Affiliation:
Institut d'Astrophysique Spatial, Université Paris Sud-11, 91405 Orsay Cedex, France email: gabriel@ias.fr
L. Abbo
Affiliation:
Osservatorio Astronomico di Torino, Pino Torinese 10025 – Italy
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Abstract

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Recent work on coronal polar plumes (Gabriel et al. 2003, 2005) has aimed at determining the outflow velocity in plume and interplume regions, using the Doppler dimming technique on oxygen VI observations by SUMER and UVCS on SOHO. By comparing observations of SOHO/EIT with plume modelling, we show that the major part of plumes is the result of chance alignments along the line-of-sight of small enhancements in intensity. This confirms the so-called curtain model. These plumes can be attributed to reconnection activity along the boundaries of supergranule cells. A second population of plumes has a lower abundance and arises from surface bright points having a particular magnetic configuration. New observations using the Hinode/EIS spectrometer are in progress, with the aim of providing further insight for this model.

Keywords

Sun: coronasolar wind
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S257: Universal Heliophysical Processes , September 2008 , pp. 145 - 149
Copyright
Copyright © International Astronomical Union 2009

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