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Planets in close-in orbit interact with the magnetized wind of their hostingstar. This magnetic interaction was proposed to be a source for enhancedemissions in the chromosphere of the star, and to participate in setting themigration time-scale of the close-in planet. The efficiency of the magneticinteraction is know to depend on the magnetic properties of the host star, ofthe planet, and on the magnetic topology of the interaction. We use a global,three-dimensional numerical model of close-in star planet systems, based on themagnetohydrodynamics approximation, to compute a grid of simulations forvarying properties of the orbiting planet. We propose a simple parametrizationof the magnetic torque that applies to the planet, and of the energy fluxgenerated by the interaction. The dependancy upon the planet properties and thewind properties are clearly identified in the derived scaling laws, which canbe used in secular evolution codes to take into account the effect of magneticinteractions in planet migration. They can also be used to estimate a potentialmagnetic source of enhanced emissions in observed close-in star-planet systems,in order to constrain observationally possible exoplanetary magnetic fields.

Assessing magnetic torques and energy fluxes in close-in star-planet systems