Observations of Unresolved Photospheric Magnetic Fields in Solar Flares Using Fe i and Cr i Lines |
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Authors: | M Gordovskyy V G Lozitsky |
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Affiliation: | 1. Jodrell Bank Centre for Astrophysics, University of Manchester, Manchester, M13 9PL, UK 2. Astronomical Observatory, Kyiv National University, Observatorna 3, Kyiv, 01053, Ukraine
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Abstract: | The structure of the photospheric magnetic field during solar flares is examined using echelle spectropolarimetric observations. The study is based on several Fe i and Cr i lines observed at locations corresponding to brightest Hα emission during thermal phase of flares. The analysis is performed by comparing magnetic-field values deduced from lines with different magnetic sensitivities, as well as by examining the fine structure of I±V Stokes-profiles’ splitting. It is shown that the field has at least two components, with stronger unresolved flux tubes embedded in weaker ambient field. Based on a two-component magnetic-field model, we compare observed and synthetic line profiles and show that the field strength in small-scale flux tubes is about 2?–?3 kG. Furthermore, we find that the small-scale flux tubes are associated with flare emission, which may have implications for flare phenomenology. |
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