The impact of mixing treatments on cloud modelling in 3D simulations of hot Jupiters

Christie, Duncan; Mayne, Nathan J.; Lines, Stefan; Parmentier, Vivien; Manners, James; Boutle, Ian; Drummond, Benjamin; Evans, T. M.; Sing, David K.; Koháry, K.

doi:10.1093/mnras/stab2027

Cited by 34 publications

(40 citation statements)

References 95 publications

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“…Different spectra could have an impact on the energy deposition in the atmosphere, as for Proxima Centauri b (Lefèvre et al 2021). In hot Jupiter cloud studies, the moment formalism is sometimes used in microphysical modeling (Lee et al 2016;Lines et al 2018), allowing the particle number density to be then determined, as well as the different particle size distributions (Christie et al 2021). Charnay et al (2018) showed a strong gravity effect on the chemistry and microphysics and the overall color.…”

Section: Discussionmentioning

confidence: 99%

Cloud-convection Feedback in Brown Dwarf Atmospheres

Lefèvre¹,

Tan²,

Lee

et al. 2022

ApJ

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Numerous observational evidence has suggested the presence of active meteorology in the atmospheres of brown dwarfs. A near-infrared brightness variability has been observed. Clouds have a major role in shaping the thermal structure and spectral properties of these atmospheres. The mechanism of such variability is still unclear, and neither 1D nor global circulation models can fully study this topic due to resolution. In this study, a convective-resolving model is coupled to gray-band radiative transfer in order to study the coupling between the convective atmosphere and the variability of clouds over a large temperature range with a domain of several hundred kilometers. Six types of clouds are considered, with microphysics including settling. The clouds are radiatively active through the Rosseland mean coefficient. Radiative cloud feedback can drive spontaneous atmospheric variability in both temperature and cloud structure, as modeled for the first time in three dimensions. Silicate clouds have the most effect on the thermal structure with the generation of a secondary convective layer in some cases, depending on the assumed particle size. Iron and aluminum clouds also have a substantial impact on the atmosphere. Thermal spectra were computed, and we find the strongest effect of the clouds is the smoothing of spectral features at optical wavelengths. Compared to observed L and T dwarfs on the color–magnitude diagram, the simulated atmospheres are redder for most of the cases. Simulations with the presence of cloud holes are closer to observations.

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Section: Discussionmentioning

confidence: 99%

Cloud-convection Feedback in Brown Dwarf Atmospheres

Lefèvre¹,

Tan²,

Lee

et al. 2022

ApJ

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show abstract

“…Different spectra could have an impact on the energy deposition in the atmosphere, as for Proxima Centauri-b (Lefèvre et al, 2021). In hot jupiters cloud studies, the moment formalism is sometimes used in the microphysical modelling (Lee et al, 2016;Lines et al, 2018), allowing the particle number density to be then determine, as well as different particle size distribution Christie et al (2021). Charnay et al (2018) showed a strong gravity effect on the chemistry and microphysics and the overall color.…”

Section: Discussionmentioning

confidence: 99%

Cloud-convection feedback in brown dwarfs atmosphere

Lefèvre,

Tan,

Lee

et al. 2022

Preprint

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Numerous observational evidence has suggested the presence of active meteorology in the atmospheres of brown dwarfs. A near-infrared brightness variability has been observed. Clouds have a major role in shaping the thermal structure and spectral properties of these atmospheres. The mechanism of such variability is still unclear and both 1D and global circulation model cannot fully study this topics due to resolution. In this study, a convective resolving model is coupled to grey-band radiative transfer in order to study the coupling between the convective atmosphere and the variability of clouds over a large temperature range with a domain of several hundreds of kilometers. Six types of clouds are considered, with microphysics including settling. The clouds are radiatively active using Rosseland mean coefficient. Radiative cloud feedback can drive spontaneous atmospheric variability in both temperature and cloud structure, as modeled for the first time in three dimensions. Silicate clouds have the most effect of the thermal structure with the generation of a secondary convective layer in some cases, depending on the assumed particle size. Iron and Aluminum clouds also have a substantial impact on the atmosphere. Thermal spectra were computed, and we find the strongest effect of clouds is the smoothing of spectral features at optical wavelengths. Compared to observed L and T dwarfs on color-magnitude diagram, the simulated atmospheres are redder for most of the cases. The simulations with the presence of cloud holes are closer to the observations.

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“…In addition, several 3D climate models include additional physical processes, which are thought to be important for the understanding of exoplanet atmospheres: clouds (Lee et al 2016;Lines et al 2019;Parmentier et al 2021;Roman et al 2021), photochemical hazes (Steinrueck et al 2021), disequilibrium chemistry (Agúndez et al 2014a;Drummond et al 2018b;Mendonça et al 2018a;Baeyens et al 2021), and magnetic fields (Rogers & Showman 2014). Cloud modeling in 3D climate models ranges from detailed kinetic modeling (e.g., Lee et al 2016) to simple but efficient parametrization (e.g., Roman et al 2021;Christie et al 2021).…”

Section: Versatile Fast 3d Gcm With Non-gray Radiative Transfermentioning

confidence: 99%

Exploring the deep atmospheres of HD 209458b and WASP-43b using a non-gray general circulation model

Carone¹,

Decin²,

Jørgensen³

et al. 2022

Preprint

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Simulations with a 3D general circulation model (GCM) suggest that one potential driver behind the observed radius inflation in hot Jupiters may be the downward advection of energy from the highly irradiated photosphere into the deeper layers. Here, we compare dynamical heat transport within the non-inflated hot Jupiter WASP-43b and the canonical inflated hot Jupiter HD 209458b, with similar effective temperatures. We investigate to what extent the radiatively driven heating and cooling in the photosphere (at pressures smaller than 1 bar) influence the deeper temperature profile (at pressures between 1 to 700 bar). Our simulations with the new non-gray 3D radiation-hydrodynamical model expeRT/MITgcm show that the deep temperature profile of WASP-43b is associated with a relatively cold adiabat. The deep layers of HD 209458b, however, do not converge and remain nearly unchanged regardless of whether a cold or a hot initial state is used. Furthermore, we show that different flow structures in the deep atmospheric layers arise. There, we find that WASP-43b exhibits a deep equatorial jet, driven by the relatively fast tidally locked rotation of this planet (0.81 days), as compared to HD 209458b (3.47 days). However, by comparing simulations with different rotation periods, we find that the resulting flow structures only marginally influence the temperature evolution in the deep atmosphere, which is almost completely dominated by radiative heating and cooling. Furthermore, we find that the evolution of deeper layers can influence the 3D temperature structure in the photosphere of WASP-43b. Thus, dayside emission spectra of WASP-43b may shed more light onto the dynamical processes occurring at greater depths.

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The impact of mixing treatments on cloud modelling in 3D simulations of hot Jupiters

Cited by 34 publications

References 95 publications

Cloud-convection Feedback in Brown Dwarf Atmospheres

Cloud-convection Feedback in Brown Dwarf Atmospheres

Cloud-convection feedback in brown dwarfs atmosphere

Exploring the deep atmospheres of HD 209458b and WASP-43b using a non-gray general circulation model

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