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A 3D fully self-consistent multi-fluid hydrodynamic aeronomy model is appliedto simulate the hydrogen-helium expanding upper atmosphere of the hot JupiterHD189733b, and related absorption in the Lya line and the 10830 A line ofmetastable helium. We studied the influence of a high-energy stellar flux,stellar wind, and Lya cooling to reproduce the available observations. We foundthat to fit the width of the absorption profile in 10830 A line the escapingupper atmosphere of planet should be close to the energy limited escapeachieved with a significantly reduced Lya cooling at the altitudes with HIdensity higher than 3*10^6 cm^-3. Based on the preformed simulations, weconstrain the helium abundance in the upper atmosphere of HD189733b by a ratherlow value of He/H~0.005. We show that under conditions of a moderate stellarwind similar to that of the Sun the absorption of Lya line takes place mostlywithin the Roche lobe due to thermal broadening at a level of about 7%. At anorder of magnitude stronger wind, a significant absorption of about 15% at highblue shifted velocities of up to 100 km/s is generated in the bowshock region,due to Doppler broadening. These blue shifted velocities are still lower thanthose (~200 km/s) detected in one of the observations. We explain thedifferences between performed observations, though not in all the details, bythe stellar activity and the related fluctuations of the ionizing radiation (incase of 10830 A line), and stellar wind (in case of Lya line).

Global 3D simulation of the upper atmosphere of HD189733b and absorption in metastable HeI and Ly{\alpha} lines