Exoplanet Chemistry

Abstract

The terrestrial and gas-giant planets in our solar system may represent some prototypes for planets around other stars; the exoplanets because most stars have similar overall elemental abundances as our sun. The solar system planets represent at least four chemical planet types, depending on the phases that make them: Terrestrial-like planets made of rock (metal plus silicates), Plutonian planets made of rock and ice, Neptunian giant planets of rocky, icy with low H and He contents, and Jovian gas-giant planets of rocky, icy planets with near-solar H and He contents. The planetary compositions are linked to the chemical fractionation in the planetary accretion disks. Chemical tracers of these fractionations are described. Many known exoplanets are gas-giant planets with up to several Jupiter-masses and their atmospheric chemistry is compared to that of brown dwarfs. Exoplanets in close orbits around their host stars may resemble hot brown dwarfs (L-dwarfs). Planets receiving less radiation form their host may compare more to the methane-rich T dwarfs. The cloud layers resulting from condensation of oxides, metal, sulfides, and salts in these hot and cool gas giant planets and their chemical tracers are described.

33 pages, 8 figures, 2 tables, in: Formation and Evolution of Exoplanets, R. Barnes (ed.), Wiley, Berlin, in press

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Cited by in corpus (31)

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• HST hot Jupiter Transmission Spectral Survey: A detection of Na and strong optical absorption in HAT-P-1b
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• High temperature condensate clouds in super-hot Jupiter atmospheres
• Retrieval of atmospheric properties of cloudy L dwarfs
• Planet-forming material in a protoplanetary disc: the interplay between chemical evolution and pebble drift
• HST hot-Jupiter transmission spectral survey: Haze in the atmosphere of WASP-6b
• Chemical Kinetics on Extrasolar Planets
• Where is the Water? Jupiter-like C/H ratio but strong H${}_2$O depletion found on $\tau$ Boötis b using SPIRou
• The optical transmission spectrum of the hot Jupiter HAT-P-32b: clouds explain the absence of broad spectral features?
• Cloud busting: enstatite and quartz clouds in the atmosphere of 2M2224-0158
• Planetesimal Compositions in Exoplanet Systems
• 1D atmospheric study of the temperate sub-Neptune K2-18b
• Modeling the effects of inhomogeneous aerosols on the hot Jupiter Kepler-7b's atmospheric circulation
• HST PanCET program: A Cloudy Atmosphere for the promising JWST target WASP-101b
• From cold to hot irradiated gaseous exoplanets: Toward an observation-based classification scheme
• The carbon-to-oxygen ratio: implications for the spectra of hydrogen-dominated exoplanet atmospheres
• Exploring the link between star and planet formation with Ariel
• Evidence for chromium hydride in the atmosphere of Hot Jupiter WASP-31b
• Atmospheric properties of AF Lep b with forward modeling
• First Observations of the Brown Dwarf HD 19467 B with JWST
• Fingerprints of the protosolar cloud collapse in the Solar System I: Distribution of presolar short-lived ${}^{26}$Al
• Disentangling protoplanetary disk gas mass and carbon depletion through combined atomic and molecular tracers
• H2-Induced Pressure Broadening and Pressure Shift in the P-Branch of the v3 Band of CH4 from 300 to 700 K
• Near-UV transit photometry of HAT-P-32 b with the LBT: Silicate aerosols in the planetary atmosphere
• GEMS JWST: Transmission spectroscopy of TOI-5205b reveals significant stellar contamination and a metal-poor atmosphere
• Exploring the Diversity of Jupiter-Class Planets (Discussion Meeting Contribution)
• Effect of Longitudinally Varying Cloud Coverage on Visible Wavelength Reflected-Light Exoplanet Phase Curves