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We investigate the thermal response of the atmosphere of a solar-type star toan electron beam injected from a hot Jupiter by performing a 1-dimensionalmagnetohydrodynamic numerical experiment with non-linear wave dissipation,radiative cooling, and thermal conduction. In our experiment, the stellaratmosphere is non-rotating and is modelled as a 1-D open flux tube expandingsuper-radially from the stellar photosphere to the planet. An electron beam isassumed to be generated from the reconnection site of the planet'smagnetosphere. The effects of the electron beam are then implemented in oursimulation as dissipation of the beam momentum and energy at the base of thecorona where the Coulomb collisions become effective. When the sufficientenergy is supplied by the electron beam, a warm region forms in thechromosphere. This warm region greatly enhances the radiative fluxescorresponding to the temperature of the chromosphere and transition region. Thewarm region can also intermittently contribute to the radiative flux associatedwith the coronal temperature due to the thermal instability. However, owing tothe small area of the heating spot, the total luminosity of the beam-inducedchromospheric radiation is several orders of magnitude smaller than theobserved Ca II emissions from HD 179949.

Thermal Response of A Solar-like Atmosphere to An Electron Beam from A Hot Jupiter: A Numerical Experiment