2012
DOI: 10.1051/0004-6361/201219310
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Abstract: Context. The atmosphere of hot Jupiters can be probed by primary transit and secondary eclipse spectroscopy. Owing to the intense UV irradiation, mixing, and circulation, their chemical composition is maintained out of equilibrium and must be modeled with kinetic models. Aims. Our purpose is to release a chemical network and the associated rate coefficients, developed for the temperature and pressure range relevant to hot Jupiters atmospheres. Using this network, we study the vertical atmospheric composition o… Show more

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Cited by 219 publications
(573 citation statements)
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References 184 publications
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“…The characterization of hot Jupiter atmospheres has motivated the development of one dimensional models that include thermochemical kinetics, diffusion, and photochemistry, and that aim at describing the chemical behaviour and composition of such atmospheres in the vertical direction (Zahnle et al 2009;Line et al 2010;Moses et al 2011;Kopparapu et al 2012;Venot et al 2012). These models indicate that chemical equilibrium is attained deep in the atmosphere, although the chemical composition of the layers typically sampled by transit observations, in the 1 bar to 0.01 mbar pressure regime, is maintained out of equilibrium due to two major disequilibrium processes.…”
Section: Introductionmentioning
confidence: 99%
“…The characterization of hot Jupiter atmospheres has motivated the development of one dimensional models that include thermochemical kinetics, diffusion, and photochemistry, and that aim at describing the chemical behaviour and composition of such atmospheres in the vertical direction (Zahnle et al 2009;Line et al 2010;Moses et al 2011;Kopparapu et al 2012;Venot et al 2012). These models indicate that chemical equilibrium is attained deep in the atmosphere, although the chemical composition of the layers typically sampled by transit observations, in the 1 bar to 0.01 mbar pressure regime, is maintained out of equilibrium due to two major disequilibrium processes.…”
Section: Introductionmentioning
confidence: 99%
“…The relative importance of thermochemical equilibrium, photochemistry, and transport-induced quenching in controlling the atmospheric composition largely depends on the thermal structure of the planets. In the case of the hotter HD209458b, deviations from the equilibrium are less noticeable than for HD189733b (Moses et al 2011;Venot et al 2012). …”
Section: Hot and Warm Jupiters And Neptunesmentioning
confidence: 88%
“…Examples of atmospheric modelling, including transport-induced quenching and photochemistry, have been developed by Moses et al (2011) and Venot et al (2012) for HD209458b and HD189733b. For both planets, CH 4 and NH 3 are enhanced with respect to their equilibrium abundances due to vertical transport-induced quenching, but are dissociated by photochemistry at higher altitude, leading, in particular, to the formation of C 2 H 2 and HCN.…”
Section: Hot and Warm Jupiters And Neptunesmentioning
confidence: 99%
“…EChO extends these methods to exoplanets: the reliable determination of the spectrum in reflected versus thermal range will provide a powerful tool for classifying the dynamical activity of exoplanets. [178]. For HD 189733b, one can clearly notice the higher sensitivity to photolyses and vertical mixing, with all species affected, except the main reservoirs, H 2 , H 2 O, CO, and N 2 .…”
Section: Energy Budget: Heating and Cooling Processesmentioning
confidence: 90%
“…In some of the known hot-Jupiters, CH 4 and NH 3 are expected to be enhanced with respect to their equilibrium abundances due to vertical transport-induced quenching. These species should be dissociated by photochemistry at higher altitude, leading, in particular, to the formation of C 2 H 2 and HCN on the day side [118,178]. EChO can address these open questions, by deriving the abundances of both key and minor molecular species, with mixing ratios down to 10 −5 to 10 −7 ( Fig.…”
Section: The Chemistry Of Gaseous Planets' Atmospheresmentioning
confidence: 99%