Investigation of exoplanetary magnetic fields and their role in evolution of planetary systems is closely connected with the study of the whole complex of stellar - planetary interactions, including consideration of influences of stellar radiation and plasma flows, e.g., stellar wind, coronal mass ejections (CMEs), on the planetary environments. Magnetic fields form planetary magnetospheres. These act as an obstacle interacting with the stellar wind, declining it, and protecting planetary ionospheres and upper atmospheres against the direct impact of stellar plasmas and energetic particles (e.g., cosmic rays). The stellar X-ray/EUV (XUV) radiation and the stellar wind result in ionization, heating, chemical modification, and slow erosion of the planetary upper atmospheres throughout their lifetime.
The major goal of this subproject consists in the investigation of key factors and physical mechanisms which determine the structure, topology and dynamics of an exoplanetary magnetosphere. In the course of the development of a general model of an exoplanetary magnetosphere, the specifics of exoplanetary conditions, such as intensive escape of the planetary atmospheric material heated and ionized by the stellar X-ray/EUV (XUV) radiation and formation of an equatorial current-carrying plasma disk will be consequently taken into account.