Magnetic field dynamics based on SOHO/MDI data in the region of flares related to halo coronal mass ejections

Variations in the photospheric magnetic field in the region of solar flares, related to halo coronal mass ejections (HCMEs) with velocities V > 1500, 1000 < V < 1500, and V < 650 km/s, have been studied based on SOHO/MDI data. Using data with a time resolution of 96 min, it has been indicated that on average the aOE (c) B (L)> and aOE (c)|B (L)|> field characteristics increase nonmonotonically during 1-1.5 days before a flare and decrease during 0.5-1 days after a flare for groups of ejections with V > 1000 km/s for all considered HCME groups. Angle brackets designate averaging of the measured B (L) magnetic field component and its magnitude |B (L)| within an area with specified dimensions and the center coincident with the projection onto the region where the flare center field is measured. It has been established that a solar flare related to an HCME originates when the aOE (c) B (L)> and aOE (c)|B (L)|> values are larger than the boundary values in the flare region. Based on 1-min data, it has been found for several HCMEs with V > 1500 km/s that the beginning of powerful flares related to ejections is accompanied by rapid impulsive or stepped variations in aOE (c) B (L)> and aOE (c)|B (L)|> near the center of a flare with a size of approximately 4.5A degrees. It has been established that the HCME velocity positively correlates with the |aOE (c) B (L)>| value at the flare onset.