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The identification of possible sources of electromagnetic emissions in exoplanetary magnetospheres and the estimation of their efficiency, as well as potential detectability, is a challenging task of the present day theoretical astrophysics. It is closely related with the understanding and consistent description of the key physical processes in the nearby exoplanetary space plasmas, and requires first of all an appropriate model of an exoplanetary magnetosphere. A comparative look at physical conditions in known and well measured magnetospheres of the solar system planets and those expected by exoplanets, shows that a direct application of the scenarios and views developed for the solar system planets to exoplanets, in spite of certain importance, may not always correctly reflect the specifics of the exoplanets. This first of all concerns the case of the so-called Hot Jupiters – giant exoplanets, orbiting close to their host stars. The existence, power efficiency, and detectability of various sources of electromagnetic emission in the magnetospheres of Hot Jupiters are nowadays widely investigated. In that respect, we present here a generalized model of a Hot Jupiter large scale magnetosphere and consider several phenomena which might influence the exoplanetary radiation. Our approach is based on a combination of two kinds of models: 1) a generalized paraboloid magnetosphere model (PMM), which calculates a large-scale magnetosphere topology produced by the whole variety of magnetic field and electric current sources, e.g., planetary magnetic dipole, magnetopause and magnetotail currents, etc.; and 2) a 2D multi–fluid MHD model of the upper atmosphere of a planet, heated and ionized by the stellar XUV radiation, which incorporates the basic hydrogen photochemistry, gravitational and rotational forces, and takes into account a realistic solar-type XUV spectrum. A key feature of the specific conditions in the magnetosphere of a close–orbit giant exoplanet, which we consequently take into consideration in our modeling, consists in the presence of an expanding atmospheric material which forms a kind of escaping planetary wind (PW), not typical for the solar system planets. ∗ Space Research Institute, Austrian Academy of Sciences, Graz, Austria † Institute of Laser Physics SB, Russian Academy of Sciences, Novosibirsk, Russia ‡ Skobeltsyn Institute of Nuclear Physics, Lomonosov Moscow State University, Moscow, Russia

Magnetospheres of Hot Jupiters: On the physical phenomena potentially observable in radio (abstract)