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

TL;DR

This study uses 3D radiation hydrodynamic simulations to model the stellar wind interaction with GJ 436b's escaping atmosphere, aiming to match Ly$ ext{a}$ absorption data and explain the lack of H$ ext{a}$ absorption.

Contribution

It provides the first detailed simulation-based constraints on stellar wind properties and planetary mass loss rates for GJ 436b, aligning models with observational Ly$ ext{a}$ data.

Findings

Stellar wind velocity around 250-460 km/s

Mass loss rate of the planet approximately 6-10 billion grams per second

No significant H$ ext{a}$ absorption detected in models, consistent with observations

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 $\sim56\%$ 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 $[3-4]\times10^5$ 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$\alpha$ line in agreement with the observations.