For five flares we have considered magnetic fields, measured in the flaring region and underlying sunspots. Main results:
a) magnetic field in flare is longitudinal, buf it is mainly transversal in fhe sunspol which the flare is situated on;
b) magnetic field strengths measured by Zeeman splitting of Ihe emission lines ol Fel, D1, and D-2 Nal, D3 Hel and Hα reach 1000-3000G, offen exeeeds ones determined by absorption lines in underlying sunspols;
e) it appears fhat in flare the magnetic field changes slowly wifh heighf, so far as its vaues estimated by emission lines of helium, hydrogen and metal are approximately equal.