Vertical inhomogenuity of the magnetic field in the solar flares

Details Vertical inhomogenuity of the magnetic field in the solar flares Vertical inhomogenuity of the magnetic field in the solar flares

Apr 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005ysc..conf...75o&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

The magnetic field is of primary importance in the physics of the Sun and Solar flare. We present the results of investigation of the solar flares of 25 October 2003 and 5 November 2004. The Echelle Zeeman-spectrograms of the flare were obtained on horizontal solar telescope of Astronomical Observatory of Kyiv Shevchenko University. Ten spectral lines of FeI, FeII, ScII and CrII were investigated to diagnose the small-scale magnetic field structures. We compared the data for 2 photometrical sections of these lines. It was shown, that magnetic field range was from 100 G to about 1000 G for both flares. There is an evidence on the spatially unresolved magnetic field sructure with kG local magnetic fields. We have built the dependence of magnetic fields and height formation for both flares. This proves the existence of the middle photosphere level (250-300 km), where the change of the height gradient sign of the magnetic field is observed.

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