Astronomy and Astrophysics – Astronomy
Scientific paper
Aug 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...3e...9l&link_type=abstract
Solar Active Regions and 3D Magnetic Structure, 26th meeting of the IAU, Joint Discussion 3, 16-17 August, 2006, Prague, Czech R
Astronomy and Astrophysics
Astronomy
Scientific paper
Two solar flares, on July 19, 2000 and August 4, 2005 of importance M6.4/3N and C8.4/1N, respectively, were studied using the echelle Zeeman spectrograms obtained with horizontal solar telescope at the Astronomical Observatory of Kyiv Shevchenko National University. The Stokes I ± V profiles were compared for about ten lines of FeI, FeII, CrII, SrII and TiII. The direct magnetic field measurements using the `center of gravity' method had shown the non-monotonous magnetic field gradient in area of first flare contrary to usual weak negative gradient outside flare emission. Semi-empirical models of flares were calculated close to maximums using Baranovsky's (1993) program are in good agreement with these direct measurements. In particular, for flare of July, 2000, a very narrow (≤ 100 km) and sharp magnetic field peak at photospheric level (lg τ[5 ]≈ -2) was discovered. This peculiarity indicates likely the local magnetic field amplification due to any specific process during the flare. Once more interesting detail is two discrete hot flare layers related to the middle photosphere and temperature minimum zone. The turbulent velocities had one or two peaks placed close to named peaks of temperature. In more weak flare on August 4, 2005 the magnetic field increased along with depth of the photosphere without peculiarities. Baranovsky E.A. Semiempirical LTE modelling of solar photosphere layers.I. Theoretical background. Contrib. Astron. Obs. Skalnate Pleso. 1993. V.23. P.107-117.
Kurochka E. V.
Lozitsky V. G.
Osyka O. B.
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