Hostname: page-component-78c5997874-xbtfd Total loading time: 0 Render date: 2024-11-13T10:43:03.682Z Has data issue: false hasContentIssue false
  • English
  • Français

Plasma dynamics in the polar coronal plumes

Published online by Cambridge University Press:  01 November 2006

N.-E. Raouafi ,
J. W. Harvey  and
S. K. Solanki
N.-E. Raouafi
Affiliation:
National Solar Observatory, Tucson, AZ 85719, USA email: nraouafi@nso.edu
J. W. Harvey
Affiliation:
National Solar Observatory, Tucson, AZ 85719, USA email: nraouafi@nso.edu
S. K. Solanki
Affiliation:
Max-Planck-Institut für Sonnensystemforschung, 37191Katlenburg-Lindau, Germany
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We use the spectral shapes of the EUV line profiles to study the plasma dynamics, acceleration and heating, in polar plumes (PP). We find that the observed profiles are reproduced fairly well when considering low plume wind speeds and velocity turbulence $(\alpha_S)$ at low altitudes followed by a rapid acceleration and heating of the plasma to reach the properties of inter-plumes (IP) by $\approx3-4~R_\odot$. We also find that plumes very close to the pole give narrow profiles at all heights that are not observed above $\approx2.5~R_\odot$. This suggests a tendency for plume footpoints to lie more than 10° away from the pole. High resolution magnetograms of SOLIS and EUV images support this hypothesis.

Keywords

Line: profilesPlasmasSun: coronaSun: solar windSun: UV radiation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S233: Solar Activity and its Magnetic Origin , March 2006 , pp. 193 - 194
Copyright
© 2006 International Astronomical Union