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Since the first discovery of an extrasolar planetary system more than adecade ago, hundreds more have been discovered. Surprisingly, many of thesesystems harbor Jupiter-class gas giants located close to the central star, atdistances of 0.1 AU or less. Observations of chromospheric 'hot spots' thatrotate in phase with the planetary orbit, and elevated stellar X-rayluminosities,suggest that these close-in planets significantly affect thestructure of the outer atmosphere of the star through interactions between thestellar magnetic field and the planetary magnetosphere. Here we carry out thefirst detailed three-dimensional MagnetoHydroHynamics (MHD) simulationcontaining the two magnetic bodies and explore the consequences of suchinteractions on the steady-state coronal structure. The simulations reproducethe observable features of 1) increase in the total X-ray luminosity, 2)appearance of coronal hot spots, and 3) phase shift of these spots with respectto the direction of the planet. The proximate cause of these is an increase inthe density of coronal plasma in the direction of the planet, which preventsthe corona from expanding and leaking away this plasma via a stellar wind. Thesimulations produce significant low temperature heating. By including dynamicaleffects, such as the planetary orbital motion, the simulation should betterreproduce the observed coronal heating.

Interactions of the magnetospheres of stars and close-in giant planets