# Modeling the Ly$\alpha$ transit absorption of the hot Jupiter HD 189733b

## TL;DR

This study models the Lyα transit absorption of hot Jupiter HD 189733b, showing that atmospheric broadening dominates the absorption signal and that typical stellar activity conditions can explain observed variations.

## Contribution

The paper combines 1D hydrodynamic and 3D MHD models to analyze how stellar XUV and wind variations affect Lyα absorption, highlighting the dominance of atmospheric broadening over ENA contributions.

## Key findings

- Lyα absorption can be explained by typical stellar activity conditions.
- Atmospheric broadening dominates the Lyα transit signature.
- ENAs have negligible impact on the absorption in this model.

## Abstract

Hydrogen-dominated atmospheres of hot exoplanets expand and escape due to the intense heating by the X-ray and extreme ultraviolet (XUV) irradiation of their host stars. Excess absorption of neutral hydrogen has been observed in the Ly$\alpha$ line during transits of several close-in exoplanets, indicating such extended atmospheres. For the hot Jupiter HD 189733b, this absorption shows temporal variability. Variations in stellar XUV emission and/or stellar wind conditions have been invoked to explain this effect. We apply a 1D hydrodynamic upper atmosphere model and a 3D MHD stellar wind flow model to study the effect of variations of the stellar XUV and wind conditions on the neutral hydrogen distribution, including the production of energetic neutral atoms (ENAs), and the related Ly$\alpha$ transit signature. We obtain comparable, albeit slightly higher Ly$\alpha$ absorption as observed in 2011 with a stellar XUV flux of $1.8\times10^4$ erg cm$^{-2}$ s$^{-1}$, rather typical activity conditions for this star. Flares similar to the one observed 8 h before the transit are unlikely to have caused a significant modulation of the transit signature. The resulting Ly$\alpha$ absorption is dominated by atmospheric broadening, whereas the contribution of ENAs is negligible, as they are formed inside the bow shock from decelerated wind ions that are heated to high temperatures. Thus, within our modeling framework and assumptions, we find an insignificant dependence on the stellar wind parameters. Since the transit absorption can be modeled with typical stellar XUV and wind conditions, it is possible that the non-detection of the absorption in 2010 was affected by less typical stellar activity conditions, such as a very different magnitude and/or shape of the star's spectral XUV emission, or temporal/spatial variations in Ly$\alpha$ affecting the determination of the transit absorption.