Spectropolarimetry Of The Footpoints Of A C-class Flare In The Chromosphere

Details Spectropolarimetry Of The Footpoints Of A C-class Flare In The Chromosphere Spectropolarimetry Of The Footpoints Of A C-class Flare In The Chromosphere

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011spd....42.0308k&link_type=abstract

American Astronomical Society, SPD meeting #42, #3.08; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

Flares are well-known solar phenomena but have rarely been imaged in high resolution polarimetry and even less often in the chromosphere. We observed the declining phase of a C-class flare in NOAA 10940 on January 29, 2007 with the IBIS instrument (0.17"/px), taking quasi-simultaneous spectropolarimetric images in the chromosphere (8542 [[Unable to Display Character: Ǻ]]) and in the photosphere (6302 [[Unable to Display Character: Ǻ]]).
Only the inner wings and core of the chromospheric line are seen to brighten in IBIS, the underlying photosphere remaining undisturbed. TRACE images reveal the connectivity of the chromospheric flaring plasma to the overlying corona: IBIS fortuitously captured the chromospheric flares associated with both footpoints of a loop systems seen in TRACE.
Our hour-long image sequence shows the evolution and weakening of the chromospheric flare, and reveals unresolved opposite magnetic field components with large velocities with respect to the average Sun. In the chromosphere, we find redshifted components but in the photosphere we see observe blueshifts. We will present high resolution movies of the flaring plasma seen in both footpoints of the loop system. We will discuss the implications of these measurements for models of the storage and release of energy for this class of small flare, and possible connections to the formation of the penumbra that appears later at this location.

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