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Hot-Jupiters are subject to extreme radiation and plasma flows coming fromtheir host stars. Past ultraviolet Hubble Space Telescope observations,supported by hydrodynamic models, confirmed that these factors lead to theformation of an extended envelope, part of which lies beyond the Roche lobe. Weuse gas-dynamic simulations to study the impact of time variations in theparameters of the stellar wind, namely that of coronal mass ejections (CMEs),on the envelope of the typical hot-Jupiter HD 209458b. We consider three CMEscharacterized by different velocities and densities, taking their parametersfrom typical CMEs observed for the Sun. The perturbations in the ram-pressureof the stellar wind during the passage of each CME tear off most of theenvelope that is located beyond the Roche lobe. This leads to a substantialincrease of the mass-loss rates during the interaction with the CME. We findthat the mass lost by the planet during the whole crossing of a CME is of${\approx}10^{15}$ g, regardless of the CME taken into consideration. We alsofind that over the course of 1 Gyr, the mass lost by the planet because of CMEimpacts is comparable to that lost because of high-energy stellar irradiation.

The Influence of Coronal Mass Ejections on the Mass-loss Rates of Hot-Jupiters