Planetary Plasma Environment

Dear Colleagues,

Solar wind interaction with planetary objects in the solar system generally results in a formation of two distinct boundaries upstream the obstacle, called magnetopause (or, in the case of unmagnetized planets, rather magnetic pileup boundary) and bow shock. In the first approximation, the solar wind plasma has no access to radial distances lower than the magnetopause standoff distance, and an (induced) magnetosphere is formed. The focus of this Special Issue is the magnetospheric plasma environment around the solar system’s planetary objects. At lower altitudes, this includes the planetary ionospheres and various factors responsible for their variability, including energetic particle precipitation. Various electromagnetic wave phenomena taking place in the respective magnetospheres are also of interest, as these can ultimately be responsible for the particle energization and/or loss. At larger radial distances, the topic includes the energy coupling between solar wind and the magnetospheres, as well as studies related to the features of and the balance across distinct plasma boundaries. Theoretical and model contributions, as well as observational studies using data from both older and recent satellite missions and ground-based instruments, are envisaged.

Dr. František Němec
Guest Editor

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