Osyka O. Magnetic fields in solar flares of middle importance from data of spectral-polarized observations.

It was first found that vertical magnetic field inhomogeneity (like narrow peak with strength up to 200 mT) disappears during 10 min of flare evolution and in place of it there is the ordinary monotonous weakening of the magnetic field with a height in a photosphere. The turbulent velocities increase from 2 km/s to 5 km/s simultaneously with magnetic field transformation. Analysis of the Stokes I±V bisectors in Fe I lines shown that magnetic field strength in subtelescopic (<1 Mm) magnetic elements reachs of 450-550 mT and has opposite polarity. Horizontal magnetic field gradient is here 0.5 mT/km, i.e. in tens times more than in sunspots close to bright flare knots.