Physics
Scientific paper
Sep 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008espm...12.2.19s&link_type=abstract
"12th European Solar Physics Meeting, Freiburg, Germany, held September, 8-12, 2008. Online at http://espm.kis.uni-freiburg.de/,
Physics
Scientific paper
We analyze and interpret spectropolarimetric observations of an active region filament located close to the solar disc center, during its phase of activity. The observations are obtained in the chromospheric He I lines at 1083.0 nm. We provide novel observational results on the magnetic field measurements in solar filaments to give constraints to the theoretical models of their support in the solar corona. Our main goal is to interpret the behavior of the atmospheric parameters retrieved from the spectropolarimetric data to give a picture of the magnetic structure of the observed filament. The analysis of the observed polarization of the He I 1083.0 nm multiplet in the filament, carried out by inverting the Stokes profiles, reveals the presence of different unresolved atmospheric components of the He lines, coexisting within the resolution element (1.2 arcsec). The different components, belonging to different magnetic field lines, show supersonic up- and downflows, sometimes within the same resolution element. The He blueshifted components belong to mostly transversal field lines in the body of the filament. These field lines are found to be curving upwards on both sides. This picture suggests the presence of dipped field lines that are moving upward, carrying with them the filament material. During this movement, we also observe filament material flowing down along field lines having the same polarity as the photospheric field (i.e. they have the opposite inclination with respect to the dipped field lines). These downflows are faster at the filament end points and can reach values close to 10 times the speed of sound. The field lines are found to be almost parallel to the filament axis in the plane perpendicular to the line of sight. We use the two main theoretical models of prominence support (dip or flux rope models) to interpret the results obtained.
Lagg Andreas
Sasso Carlo
Solanki Sami K.
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