Stellar wind effect on the atmospheric escape of hot Jupiters and their Ly α and H α transits

Atmospheric escape of close-in exoplanets can be driven by high energy radiation from the host star. The planetary outflows interacting with stellar wind may generate observable transit signals that depend on strength wind. We perform detailed radiation-hydrodynamics simulations atmospheric hot Jupiters including star in a self-consistent, dynamically coupled manner. show outflow is shaped balance between its thermal pressure and ram use simulation outputs to calculate Lyman-$\alpha$ H$\alpha$ signatures. Strong winds confine decrease depth. Contrastingly, effect weak because small contribution uppermost atmosphere planet. Observing both lines important understand UV host. mass-loss rate approximately independent also discuss coronal mass ejections argue around M dwarfs significant every transit.