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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: [email protected]
Sarah E. Gibson
Affiliation:
High Altitude Observatory, NCAR, P.O. Box 3000, Boulder, CO 80307, USA email: [email protected], [email protected], [email protected]
Yuhong Fan
Affiliation:
High Altitude Observatory, NCAR, P.O. Box 3000, Boulder, CO 80307, USA email: [email protected], [email protected], [email protected]
Christian Bethge
Affiliation:
High Altitude Observatory, NCAR, P.O. Box 3000, Boulder, CO 80307, USA email: [email protected], [email protected], [email protected]
Blake Forland
Affiliation:
Metropolitan State College of Denver, P.O. Box 173362, Denver, CO 80217-3362, USA email: [email protected]
Laurel A. Rachmeler
Affiliation:
Royal Observatory of Belgium, Avenue Circulaire 3, 1180 Brussels, Belgium email: [email protected]
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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
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. 395 - 396
Copyright
Copyright © International Astronomical Union 2013 

References

Bak-Stȩślicka, U., Gibson, S. E., Fan, Y., Bethge, C., Forland, B., & Rachmeler, L. A. 2013, ApJ (Letters), 770, 28CrossRefGoogle Scholar
Fan, Y. 2010, ApJ, 719, 728CrossRefGoogle Scholar
Lemen, J. R., Title, A. M., Akin, D. J., et al. 2012, Solar Phys., 275, 17CrossRefGoogle Scholar
Tomczyk, S., Card, G. L., Darnell, T., Elmore, D. F., Lull, R.et al. 2008, Solar Phys., 247, 411Google Scholar