Studies of very hot Jupiter atmosphere with high resolution transmission spectroscopy

Presenter: Kiyoe KAWAUCHI
Recent observations have found a number of hot Jupiters, which are gas planets orbiting near a star and do not exist in the solar system. To reveal the formation scenario of hot Jupiters, it is required to gain insights for the structure and elements of the planetary atmosphere which are governed by the planet formation scenarios. In particular, alkali metal lines are one of the most important key opacity sources as the alkali metal’s wide line wings absorb almost all of the incoming stellar irradiation.
In addition, the observed transmission spectra in very-hot Jupiters (>2000K) are different from prediction from equilibrium temperature with Fortney et al. 2010. It was considered that the features of TiO/VO were large and hid the other absorption features in very-hot Jupiter. However, Na feature is detected in a few very-hot Jupiters. Owing to investigate the reason for the different absorptions, it is important to investigate more very-hot Jupiters.
We performed high-resolution transmission spectroscopy for very hot Jupiter WASP-76b with the Subaru 8.2 m telescope and the High Dispersion Spectrograph (HDS).
I will present our results and discussion which compare with the model spectra.