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We present two-dimensional multi-fluid numerical modelling of the upperatmosphere of the hot Jupiter WASP-12b. The model includes hydrogen chemistry,and self-consistently describes the expansion of the planetary upper atmosphereand mass loss due to intensive stellar irradiation, assuming a weaklymagnetized planet. We simulate the planetary upper atmosphere and itsinteraction with the stellar wind (SW) with and without the inclusion of tidalforce and consider different XUV irradiation conditions and SW parameters. Withthe inclusion of tidal force, even for a fast SW, the escaping planetarymaterial forms two streams, propagating towards and away from the star. Theatmospheric escape and related mass loss rate reaching the value of 10^12 gs^-1appear to be mostly controlled by the stellar gravitational pull. We computedthe column density and dynamics of MgII ions considering three different setsof SW parameters and XUV fluxes. The simulations enable to compute theabsorption at the position of the Mg h line and to reproduce the times ofingress and egress. In case of a slow SW and without accounting for tidalforce, the high orbital velocity leads to the formation of a shockapproximately in the direction of the planetary orbital motion. In this case,mass loss is proportional to the stellar XUV flux. At the same time, ignoringof tidal effects for WASP-12b is a strong simplification, so the scenario witha shock, altogether is an unrealistic one.

Modelling atmospheric escape and MgII near-ultraviolet absorption of the highly irradiated hot Jupiter WASP-12b