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GJ 436b and the stellar wind interaction: simulations constraints using Ly$α$ and H$α$ transits

The GJ 436 planetary system is an extraordinary system. The Neptune-size planet that orbits the M3 dwarf revealed in the Ly$α$ line an extended neutral hydrogen atmosphere. This material fills a comet-like tail that obscures the stellar disc for more than 10 hours after the planetary transit. Here, we carry out a series of 3D radiation hydrodynamic simulations to model the interaction of the stellar wind with the escaping planetary atmosphere. With these models, we seek to reproduce the $\sim56\%$ absorption found in Ly$α$ transits, simultaneously with the lack of absorption in H$α$ transit. Varying the stellar wind strength and the EUV stellar luminosity, we search for a set of parameters that best fit the observational data. Based on Ly$α$ observations, we found a stellar wind velocity at the position of the planet to be around [250-460] km s$^{-1}$ with a temperature of $[3-4]\times10^5$ K. The stellar and planetary mass loss rates are found to be $2\times 10^{-15}$ M$_\odot$ yr$^{-1}$ and $\sim[6-10]\times10^9$ g s$^{-1}$, respectively, for a stellar EUV luminosity of $[0.8-1.6]\times10^{27}$ erg s$^{-1}$. For the parameters explored in our simulations, none of our models present any significant absorption in the H$α$ line in agreement with the observations.