577 citations · 5.5k across the 93 of their papers we have counts for
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Ionized calcium in the atmospheres of two ultra-hot exoplanets WASP-33b and KELT-9b
F. Yan, N. Casasayas-Barris, K. Molaverdikhani +25
Ultra-hot Jupiters are emerging as a new class of exoplanets. Studying their chemical compositions and temperature structures will improve the understanding of their mass loss rate…
From cold to hot irradiated gaseous exoplanets: Fingerprints of chemical disequilibrium in atmospheric spectra
Karan Molaverdikhani, Thomas Henning, Paul Mollière
Almost all planetary atmospheres are affected by disequilibrium chemical processes. In this paper we introduce our recently developed Chemical Kinetic Model (\texttt{ChemKM}). We s…
Understanding the atmospheric properties and chemical composition of the ultra-hot Jupiter HAT-P-7b: I. Cloud and chemistry mapping
Ch. Helling, N. Iro, L. Corrales +10
Ultra-hot Jupiters have recently attracted interest from observers and theoreticians alike, as they provide observationally accessible test cases. We apply a hierarchical modelling…
The Need for Laboratory Measurements and Ab Initio Studies to Aid Understanding of Exoplanetary Atmospheres
Jonathan J. Fortney, Tyler D. Robinson, Shawn Domagal-Goldman +85
We are now on a clear trajectory for improvements in exoplanet observations that will revolutionize our ability to characterize their atmospheric structure, composition, and circul…
petitRADTRANS: a Python radiative transfer package for exoplanet characterization and retrieval
P. Mollière, J. P. Wardenier, R. van Boekel +3
We present the easy-to-use, publicly available, Python package petitRADTRANS, built for the spectral characterization of exoplanet atmospheres. The code is fast, accurate, and vers…
Constraining Stellar Photospheres as an Essential Step for Transmission Spectroscopy of Small Exoplanets
Benjamin V. Rackham, Arazi Pinhas, Dániel Apai +29
Transmission spectra probe the atmospheres of transiting exoplanets, but these observations are also subject to signals introduced by magnetic active regions on host stars. Here we…