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

Abstract

The GJ 436 planetary system is an extraordinary system. The Neptune-size planet that orbits the M3 dwarf revealed in the Ly$\alpha$ 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 $\sim 56\%$ absorption found in Ly$\alpha$ transits, simultaneously with the lack of absorption in H$\alpha$ 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$\alpha$ 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 $[3-4]\times 10^5$ K. The stellar and planetary mass loss rates are found to be $2\times 10^{-15}$ M${}_{\odot }$ yr${}^{-1}$ and $\sim [6-10]\times 10^9$ g s${}^{-1}$, respectively, for a stellar EUV luminosity of $[0.8-1.6]\times 10^{27}$ erg s${}^{-1}$. For the parameters explored in our simulations, none of our models present any significant absorption in the H$\alpha$ line in agreement with the observations.

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• M-dwarf's Chromosphere, Corona and Wind Connection via the Nonlinear Alfvén Wave
• Observing atmospheric escape in sub-Jovian worlds with JWST
• Atmospheric mass loss and stellar wind effects in young and old systems I: comparative 3D study of TOI-942 and TOI-421 systems