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2015 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 802, no 1, 3Article in journal (Refereed) Published
Abstract [en]

Solar prominences are clouds of cool plasma levitating above the solar surface and insulated from the million-degree corona by magnetic fields. They form in regions of complex magnetic topology, characterized by non-potential fields, which can evolve abruptly, disintegrating the prominence and ejecting magnetized material into the heliosphere. However, their physics is not yet fully understood because mapping such complex magnetic configurations and their evolution is extremely challenging, and must often be guessed by proxy from photometric observations. Using state-of-the-art spectro-polarimetric data, we reconstruct the structure of the magnetic field in a prominence. We find that prominence feet harbor helical magnetic fields connecting the prominence to the solar surface below.

Place, publisher, year, edition, pages
2015. Vol. 802, no 1, 3
Keyword [en]
polarization, Sun: chromosphere, Sun: corona, Sun: magnetic fields
National Category
Astronomy, Astrophysics and Cosmology
URN: urn:nbn:se:su:diva-116998DOI: 10.1088/0004-637X/802/1/3ISI: 000351834700003OAI: diva2:811895


Available from: 2015-05-13 Created: 2015-05-05 Last updated: 2015-05-13Bibliographically approved

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de la Cruz Rodriguez, Jaime
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Department of Astronomy
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