Physics – Space Physics
Scientific paper
Apr 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005ysc..conf...68s&link_type=abstract
12th Young Scientists' Conference on Astronomy and Space Physics, held in Kyiv, Ukraine, April 19-23, 2005, Eds.: Simon, A.; Gol
Physics
Space Physics
Scientific paper
We continue to study the fine peculiarities of the Zeeman effect in the sunspot of 25 March 1991 which was observed on horizontal solar telescope of Astronomical Observatory of Kyiv Shevchenko University. Zeeman splittings of I +V Stokes profiles of 20 spectral lines of FeI, VI, FeII, MoI, SiI, TiI and NiI were compared to diagnose the small-scale magnetic field structure in sunspot umbra. It was shown the observational evidences to the essential magnetic field inhomogeneity in both horizontal and vertical directions. First type of inhomogeneity follows from comparison of measured magnetic field values B versus Lande factors g of lines. Although the directly measured field strength B for the same place of sunspots was in range 150-650 mT, true range of field, as it follows from 'B-g' dependence, was likely wider, up to 1600 mT. Similar magnetic field strength was measured earlier by Lozitsky (1980, 1993, 1998) in solar flares and non-spot regions. In all cases such high magnetic field values should relate to the small-scale (spatiall unresolved) magnetic structures with small filling factor. Second type of inhomogeneity follows from magnetic field comparison for lines with the same or close Lande factors. This comparison shows that vertical magnetic field gradient at photospheric level of sunspot reaches about -0.8 mT/km.
Lozitsky V. V.
Salimova N.
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