Structure and evolution of the magnetic field in the solar flare of 29 march 2001

Details Structure and evolution of the magnetic field in the solar flare of 29 march 2001 Structure and evolution of the magnetic field in the solar flare of 29 march 2001

Apr 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002kfnt...18..149l&link_type=abstract

Kinematika i Fizika Nebesnykh Tel, vol. 18, no. 2, p. 149-160

Astronomy and Astrophysics

Astronomy

Scientific paper

Preliminary results on the solar flare of 29 March 2001 of importance X1.7/1B are presented. The echelle Zeeman spectrograms of the flare were obtained on the horizontal solar telescope of the Astronomical Observatory of the Kyiv Shevchenko University. Measurements of the longitudinal magnetic field strength B∥ by the "center of gravity" method showed that the field observed in the Fe I 630.25 and Fe I 630.15 lines increased during the first 8 min of the flare, including the flare peak, and systematically B∥ (630.25)> B∥ (630.15). The Stokes I and V profiles of Fe I λλ 617.33 and 602.41 lines display a correlation between the intensity fluctuations in the "red" and "violet" wings of two lines and in the adjacent continuum. There is a moderate positive correlation for Stokes I (to r = +0.54, p < 0.001), but the correlation is negative for Stokes V (to r = -0.49, p < 0.001). Taking into account that such effects were observed at large distances from line centers (to 64±), and allowing for the sign of circular polarization at these wavelengths, we can conclude the following. The observed bright H-alpha flare knot projected on a peculiar space region with a close contact of small-scale magnetic structures of opposite polarity and discrete values of field strengths, including the following ones: ±(0.1), +0.18, -0.55, -2.3, and -2.9 T. The horizontal magnetic field gradient was about 1 mT/km here.

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