Programme by Session

In this paper we describe observational and simulated properties of emission and sunquakes generated by the largest 9.3 X-class flare of the current cycle on September 6, 2017. We analyse the events and their coronal and photospheric impacts using helioseismic techniques and HMI/SDO data supplemented by atmospheric observations from GOES, RHESSI, KONUS, AIA/SDO and Hinode. We also use observations of high resolution H-alpha emission by Swedish Solar Telescope, Lyman alpha observations by Lyra/PROBA and white light (WL) emission. The radiative signatures were simulated for Balmer hydrogen and Paschen (WL) emission using full NLTE radiative transfer models for hydrogen applied to hydrodynamic atmospheres heated by particle beams. We compare the emission contributions functions and seismic responses of flaring atmosphere heated by particle beams in this flare with that of the flare of 6 September 2011 generated at the maximum and minimum of solar activity. We evaluate energies and momenta delivered to the solar surface and interior and search for possible mechanisms of sun quake generation in each case. We show that despite the both events were accompanied by the sun quakes they exhibit strikingly different characteristics. This comparison allows us to derive the important properties of energy and particle transport in flaring atmospheres at the different phases of solar activity.