Star-planet interaction through spectral lines

Abstract

The growth of spectroscopic observations of exoplanetary systems allows the possibility of testing theoretical models and studying the interaction that exoplanetary atmospheres have with the wind and the energetic photons from the star. In this work, we present a set of numerical 3D simulations of HD 209458b for which spectral lines observations of their evaporative atmosphere are available. The different simulations aim to reproduce different scenarios for the star-planet interaction. With our models, we reconstruct the Ly$\alpha$ line during transit and compare with observations. The results allow us to analyse the shape of the line profile under these different scenarios and the comparison with the observations suggests that HD209458b may have a magnetic field off less than 1 G. We also explore the behaviour of the magnesium lines for models with and without magnetic fields.

References in corpus (5)

• Atmospheric Escape from Hot Jupiters
• Improved parameters for extrasolar transiting planets
• Magnetised winds and their influence in the escaping upper atmosphere of HD 209458b
• On the sensitivity of extrasolar mass-loss rate ranges: HD 209458b a case study
• Hydrodynamical interaction of stellar and planetary winds: effects of charge exchange and radiation pressure on the observed Ly$\alpha$ absorption