Impact Linear Polarization of the H α Line Observed in a Proton Flare with the Irkutsk Large Solar Vacuum Telescope

Details Impact Linear Polarization of the H α Line Observed in a Proton Flare with the Irkutsk Large Solar Vacuum Telescope Impact Linear Polarization of the H α Line Observed in a Proton Flare with the Irkutsk Large Solar Vacuum Telescope

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008soph..249...53f&link_type=abstract

Solar Physics, Volume 249, Issue 1, pp.53-73

Physics

3

Solar Flare, Spectrograph, Impact Polarization

Scientific paper

The impulsive phase of the 23 July 2002 2B/X4.8 proton flare with a classical two-ribbon structure was observed with the Irkutsk Large Solar Vacuum Telescope (LSVT) in spectropolarimetric mode, with high spatial, spectral, and time resolution. On the basis of 49 spectrograms and 1200 spectral cuts across the flare ribbons, evidence for H α line impact polarization has been obtained. A systematic change of the Stokes Q and U parameters has been detected across the ribbons for different flare regions measured with a scanning step of 0.85″. In the eastern side of the ribbons, the degree of polarization is 4 8%; its plane is oriented toward the solar disk center (radial direction). In the western side, the polarization degree runs up to 25%, and its plane is perpendicular to the disk center direction (tangential direction). A comparison of these results with hard X-ray data (RHESSI) allows us to conclude that high-energy electron beams reached the chromosphere during this flare. The observed changes of the direction of polarization and the vanishing polarization within the ribbons mean that, at the chromospheric level, the energy of electrons remaining in the beam is about 200 eV. A shift of the peak position of polarization relative to the intensity maximum in the ribbons may result from the inclination of the electron beam axis with respect to the solar surface.

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