G. Lee

Modelling the local and global cloud formation on HD 189733b

G.L. and Ch.H. highlight the financial support of the European community under the FP7 ERC starting grant 257431.

The mineral clouds on HD 209458b and HD 189733b

We highlight financial support of the European Community under the FP7 by the ERC starting grant 257431 and by an ERC advanced grant 247060. JK acknowledges the Rosen fellowship from the Brooklyn College New York, US.

Dynamic mineral clouds on HD 189733b : I. 3D RHD with kinetic, non-equilibrium cloud formation

Observations of exoplanet atmospheres have revealed the presence of cloud particles in their atmospheres. 3D modelling of cloud formation in atmospheres of extrasolar planets coupled to the atmospheric dynamics has long been a challenge. We investigate the thermo-hydrodynamic properties of cloud formation processes in the atmospheres of hot Jupiter exoplanets. We simulate the dynamic atmosphere of HD 189733b with a 3D model that couples 3D radiative-hydrodynamics with a kinetic, microphysical mineral cloud formation module designed for RHD/GCM exoplanet atmosphere simulations. Our simulation includes the feedback effects of cloud advection and settling, gas phase element advection and depletion/replenishment and the radiative effects of cloud opacity. We model the cloud particles as a mix of mineral materials which change in size and composition as they travel through atmospheric thermo-chemical environments. All local cloud properties such as number density, grain size and material composition are time-dependently calculated. Gas phase element depletion as a result of cloud formation is included in the model. In-situ \textit{effective medium theory} and Mie theory is applied to calculate the wavelength dependent opacity of the cloud component. We present a 3D cloud structure of a chemically complex, gaseous atmosphere of the hot Jupiter HD 189733b. Mean cloud particle sizes are typically sub-micron (0.01-0.5

Dust in brown dwarfs and extra-solar planets - IV. Assessing TiO2 and SiO nucleation for cloud formation modelling

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Understanding the water emission in the mid- and far-IR from protoplanetary disks around T Tauri stars

m) at pressures less than 1 bar with hotter equatorial regions containing the smallest grains. Denser cloud structures occur near terminator regions and deeper (

EXTENDED BASELINE PHOTOMETRY OF RAPIDLY CHANGING WEATHER PATTERNS ON THE BROWN DWARF BINARY LUHMAN-16

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Dust in brown dwarfs and extrasolar planets - V. Cloud formation in carbon- and oxygen-rich environments

1 bar) atmospheric layers. Silicate materials such as MgSiO

Simulating the cloudy atmospheres of HD 209458 b and HD 189733 b with the 3D Met Office Unified Model

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Dynamic mineral clouds on HD 189733b - II. Monte Carlo radiative transfer for 3D cloudy exoplanet atmospheres: combining scattering and emission spectra

[s] are found to be abundant at mid-high latitudes, while TiO

Dust in brown dwarfs and extra-solar planets - VI. Assessing seed formation across the brown dwarf and exoplanet regimes

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