Dust in brown dwarfs - III. Formation and structure of quasi-static cloud layers

By Peter Woitke, Ch. Helling. 2004

155 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Computational Mechanics

View Paper: https://www.semanticscholar.org/paper/9334153e7fce27d58c38a32a906487706fed86d3

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In Computational Mechanics

Citations in the corpus

3D mixing in hot Jupiters atmospheres. I. Application to the day/night cold trap in HD 209458b (2013, methodology): “This velocity depends on the size of the particles, which is determined by the complex microphysics of condensation,out of the scope of this study (see Woitke & Helling 2003).”
Standing on the shoulders of giants : Trojan Earths and vortex trapping in low mass self-gravitating protoplanetary disks of gas and solids (2008, background): “As stressed by Woitke & Helling (2003), at intermediate Knudsen numbers, the true friction force yields smaller values than in both limiting cases, which is illustrated in Fig.”
Rosseland and Planck mean opacities for protoplanetary discs (2003, background): “Since here a phase-transition takes place, a supersaturated gas would be needed which results in higher molecular abundances than AF derive from their equilibrium consideration (for a discusion see e.g. Woitke & Helling 2003).”
Retrieving scattering clouds and disequilibrium chemistry in the atmosphere of HR 8799e (2020, unknown): “51 Pegasi b fellow. cloud models are described in Woitke & Helling (2004); Helling et al. (2008a); Woitke et al. (2020), Gao et al. (2018), and Powell et al. (2018).”
L and T Dwarf Models and the L to T Transition (2005, background): “Though there have been some good starts at framing the discussion of some of these components (Helling et al. 2001, 2004; Woitke & Helling 2003,2004; Ackerman & Marley 2001; Cooper et al. 2003), we believe these issues are still to be adequately addressed.”
A comparison of chemistry and dust cloud formation in ultracool dwarf model atmospheres (2008, background): “Nucleation, growth/evaporation and gravitational settling are source terms of these equations (Woitke & Helling 2003; Helling & Woitke 2006).”
Equilibrium chemistry down to 100 K (2017, unknown): “…but the concentrations of gaseous molecules are calculated in thermo-chemical equilibrium (e.g. Gail et al. 1984; Sedlmayr & Dominik 1995; Woitke & Helling 2004; Woitke 2006; Höfner & Andersen 2007; Höfner et al. 2016; Helling & Fomins 2013), following the idea that dust formation is by…”
THE 0.8–14.5 μm SPECTRA OF MID-L TO MID-T DWARFS: DIAGNOSTICS OF EFFECTIVE TEMPERATURE, GRAIN SEDIMENTATION, GAS TRANSPORT, AND SURFACE GRAVITY (2009, background): “Woitke & Helling (2003) and Helling et al. (2008a) use seed particles and nucleation to model grain growth and then allow the grains to drift into regions where they may continue growing before settling and evaporating deep in the atmosphere.”
The Transit Light Source Effect: False Spectral Features and Incorrect Densities for M-dwarf Transiting Planets (2017, background): “…& Baron 1999), with the DRIFT-PHOENIX model grids including additional physics describing the formation and condensation of mineral dust clouds (Woitke & Helling 2003, 2004; Helling & Woitke 2006; Helling et al. 2008a,b; Witte et al. 2009) that is applicable to late M dwarfs and brown dwarfs.”
Low-Temperature Opacities (2005, unknown): “The effect of removing an important species such as titanium via (for example) the gravitational settling (see Allard et al. 2001 and Woitke & Helling 2004) of solid particles can greatly affect the opacity.”
A Unified Near-Infrared Spectral Classification Scheme for T Dwarfs (2005, background): “…(Ackerman & Marley 2001), are likely to be complex functions of Teff , surface gravity, metallicity, rotation and other parameters (Helling et al. 2001, 2004; Lodders 2002; Woitke & Helling 2003, 2004); hence, substantial spectral variations among dust-dominated sources might be expected.”
A Spitzer Infrared Spectrograph Spectral Sequence of M, L, and T Dwarfs (2004, unknown): “The Ackerman & Marley cloud model predicts submicron particle sizes high above the condensation layer (as do Woitke & Helling (2004)), but these small particles do not provide enough opacity to produce a detectable effect on the model spectra.”
Planet formation bursts at the borders of the dead zone in 2D numerical simulations of circumstellar disks (2009, methodology): “We use the formula of Woitke & Helling (2003) that interpolates between Epstein and Stokes drag CD = 9Kn2C Eps D + C Stk D (3Kn + 1)2 .”
The prevalence of dust on the exoplanet HD 189733b from Hubble and Spitzer observations (2012, background): “Following Ackerman & Marley (2001) and Woitke & Helling (2003), we estimate the settling timescale by calculating the time taken for grains to cross one atmospheric scale height at their terminal fall velocity.”
Dust flow in gas disks in the presence of embedded planets (2006, unknown): “…particles that move very supersonically through the gas, the drag force becomes: fd = −Σ 3 4 √ π 8 ΩK Ts |∆v| cs ∆v. (13) A standard way to connect the supersonic to the subsonic regime is (Kwok 1975): fd = −Σ ΩK Ts √ 1 + 9π 128 |∆v|2 c2s ∆v. (14) See Woitke & Helling (2003) for the general case.”