2017/09/01 by Elyar Sedaghati, H. M. J. Boffin, Henri M. J. Boffin +10 · 2 citations
Chemistry · Physics and Astronomy · #Astro and Planetary Science #Astrobiology #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Atmosphere (unit) #Chemistry #Exoplanet #Haze #Hot Jupiter #Materials science #Metallurgy #Oxide #Physics #Planet #Stellar, planetary, and galactic studies #Titanium oxide #astro-ph.EP
paper · pdf · doi:10.1038/nature23651
published as Nature 549, 238-241 (2017) · Main article: 9 pages, 3 figures. Methods: 21 pages, 7 extended data figures, 3 extended data tables. Published in Nature
openalex publication_date 2017/09/01 · arxiv created 2017/09/13 · arxiv updated 2017/09/15 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
As an exoplanet transits its host star, some of the light from the star is absorbed by the atoms and molecules in the planet's atmosphere, causing the planet to seem bigger; plotting the planet's observed size as a function of the wavelength of the light produces a transmission spectrum. Measuring the tiny variations in the transmission spectrum, together with atmospheric modelling, then gives clues to the properties of the exoplanet's atmosphere. Chemical species composed of light elements-such as hydrogen, oxygen, carbon, sodium and potassium-have in this way been detected in the atmospheres of several hot giant exoplanets, but molecules composed of heavier elements have thus far proved elusive. Nonetheless, it has been predicted that metal oxides such as titanium oxide (TiO) and vanadium oxide occur in the observable regions of the very hottest exoplanetary atmospheres, causing thermal inversions on the dayside. Here we report the detection of TiO in the atmosphere of the hot-Jupiter planet WASP-19b. Our combined spectrum, with its wide spectral coverage, reveals the presence of TiO (to a confidence level of 7.7σ), a strongly scattering haze (7.4σ) and sodium (3.4σ), and confirms the presence of water (7.9σ) in the atmosphere.