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The spatial relation between EUV cavities and linear polarization signatures

Published online by Cambridge University Press:  06 January 2014

Urszula Bak-Stȩślicka ,
Sarah E. Gibson ,
Yuhong Fan ,
Christian Bethge ,
Blake Forland  and
Laurel A. Rachmeler
Urszula Bak-Stȩślicka
Affiliation:
Astronomical Institute, University of Wrocław, ul. Kopernika 11, 51-622 Wrocław, Poland email: bak@astro.uni.wroc.pl
Sarah E. Gibson
Affiliation:
High Altitude Observatory, NCAR, P.O. Box 3000, Boulder, CO 80307, USA email: sgibson@ucar.edu, yfan@ucar.edu, bethge@ucar.edu
Yuhong Fan
Affiliation:
High Altitude Observatory, NCAR, P.O. Box 3000, Boulder, CO 80307, USA email: sgibson@ucar.edu, yfan@ucar.edu, bethge@ucar.edu
Christian Bethge
Affiliation:
High Altitude Observatory, NCAR, P.O. Box 3000, Boulder, CO 80307, USA email: sgibson@ucar.edu, yfan@ucar.edu, bethge@ucar.edu
Blake Forland
Affiliation:
Metropolitan State College of Denver, P.O. Box 173362, Denver, CO 80217-3362, USA email: bforland@msudenver.edu
Laurel A. Rachmeler
Affiliation:
Royal Observatory of Belgium, Avenue Circulaire 3, 1180 Brussels, Belgium email: rachmeler@oma.be
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Abstract

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Solar coronal cavities are regions of rarefied density and elliptical cross-section. The Coronal Multi-channel Polarimeter (CoMP) obtains daily full-Sun coronal observations in linear polarization, allowing a systematic analysis of the coronal magnetic field in polar-crown prominence cavities. These cavities commonly possess a characteristic “lagomorphic” signature in linear polarization that may be explained by a magnetic flux-rope model. We analyze the spatial relation between the EUV cavity and the CoMP linear polarization signature.

Keywords

Sun: coronaSun: filamentsprominencesSun: infraredSun: magnetic field

References

Bak-Stȩślicka, U., Gibson, S. E., Fan, Y., Bethge, C., Forland, B., & Rachmeler, L. A. 2013, ApJ (Letters), 770, 28CrossRefGoogle Scholar
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