Magnetic fields and Fe I line profiles in the major solar flare on October 28, 2003

Details Magnetic fields and Fe I line profiles in the major solar flare on October 28, 2003 Magnetic fields and Fe I line profiles in the major solar flare on October 28, 2003

Feb 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009astl...35..136l&link_type=abstract

Astronomy Letters, Volume 35, Issue 2, pp.136-142

Astronomy and Astrophysics

Astronomy

Scientific paper

Strong (“kilogauss”) small-scale magnetic fields were detected outside a sunspot near the seismic source of the major X17.2/4B solar flare on October 28, 2003. Echelle Zeeman spectrograms of the flare were obtained with the horizontal solar telescope at the Astronomical Observatory of the Taras Shevchenko Kiev National University. Analysis of the Stokes I ± V profiles for the Fe I 5232.9, 5247.1, 5250.2, and 5397.1 Å lines has revealed a number of characteristic spectral features. These are indicative of both background fields with a strength of ≈300 G and small-scale fields with a strength of 1300 3100 G. Evidence for the presence of another small-scale field component of opposite polarity with a strength of 8 10 kG has been found. A redshift (downflow) with a velocity of 1 km s-1 was observed in the latter component.

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