Physics
Scientific paper
May 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994soph..151..319l&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 151, no. 2, p. 319-331
Physics
9
Magnetic Anomalies, Solar Flares, Stokes Law Of Radiation, Sunspots, Emission Spectra, Line Spectra, Magnetic Flux, Nonuniform Magnetic Fields, Polarimetry, Solar Spectrometers, Spectral Signatures, Zeeman Effect
Scientific paper
I +/- V profiles of the Fe I 5247 and 5250 lines in the 2B flare of June 16, 1989 have been analyzed. A bright knot of the flare outside the sunspot where the central intensity of H alpha reached a peak value of 1.4 (relative to the continuum) has been explored. The Fe I 5250/Fe I 5247 magnetic line ratio based on the Stokes V peak separations of these lines at five evolutionary phases of the flare (including the start of the flare, the flash phase, the peak and 16 min after the peak) has been analyzed. It was found that the Stokes V peak separation for the Fe I 5250 line was systematically larger than that of the Fe I 5247 line. This is evidence for the presence in the flare of small-scale flux tubes with kG fields. The flux tube magnetic field strength was about 1.1 kG at the start of the flare and during the flash phase, 1.55 kG during the peak, and 1.38 kG 16 min after the peak. The filling factor, alpha, appears to decrease monotonically during the flare.
Lozitska Natalia
Lozitskij Vsevolod
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