A new insight into the energy release and transport in solar flares

The SOHO/MDI observations of fast magnetic field variations associated with flares reveal a close temporal correlation of the irreversible magnetic field changes occurring in the bipolar flare region with the temporal behaviour of hard and soft X-ray emission. These are expected to be accounted for a primary magnetic energy release during the flare event. There are also reversible changes of magnetic field, called earlier as 'magnetic transients', occurring in some unipolar flare regions. These changes are likely to reflect the mechanisms of energy transport into deeper atmospheric layers by charged particles (electrons and/or protons). These 'transient' magnetic field changes are also accompanied by Moreton waves in the chromosphere and EIT waves in the corona. The attempt to interpret these events using our previous kinetic models for beam electrons revealed that the energy momentum of electron beam delivered to the photospheric levels is marginally close to the limit derived from the recent solar quake observations. This encourages to consider a neutralised beam as the most possible source of both magnetic and helioseismic waves.