2004
DOI: 10.1051/0004-6361:20034514
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Dust in brown dwarfs

Abstract: Abstract. Dust formation in brown dwarf atmospheres is studied by utilising a model for driven turbulence in the mesoscopic scale regime. We apply a pseudo-spectral method where waves are created and superimposed within a limited wavenumber interval. The turbulent kinetic energy distribution follows the Kolmogoroff spectrum which is assumed to be the most likely value. Such superimposed, stochastic waves may occur in a convectively active environment. They cause nucleation fronts and nucleation events and ther… Show more

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Cited by 56 publications
(57 citation statements)
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“…And only a tiny fraction of the energy can be expected to be transformed into pressure waves under these nearly incompressible low-Mach-number conditions. Therefore, based on our simulations we cannot justify the assumption of almost sonic pressure waves in the atmospheres of brown dwarfs as made in Helling et al (2004).…”
Section: Comparison With Previous Simulationsmentioning
confidence: 78%
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“…And only a tiny fraction of the energy can be expected to be transformed into pressure waves under these nearly incompressible low-Mach-number conditions. Therefore, based on our simulations we cannot justify the assumption of almost sonic pressure waves in the atmospheres of brown dwarfs as made in Helling et al (2004).…”
Section: Comparison With Previous Simulationsmentioning
confidence: 78%
“…However, the overshoot scale height decreases rapidly with T eff and remains small (H v ≈ 0.28 H p ) from about 2200 K on, indicating that this type of overshoot is insignificant for material mixing within the forsterite cloud layers. On the other hand, for dust types that form at slightly higher temperatures (around 2000 K) as discussed e.g., in Helling et al (2004) the mixing caused by convective overshoot can play a role.…”
Section: Exponential Overshootmentioning
confidence: 99%
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“…Dynamical processes in the atmospheres of individual objects ultimately control the growth and sedimentation of condensates and the optical properties of the various cloud decks expected in these atmospheres (e.g., Helling et al 2001Helling et al , 2004Woitke & Helling 2003). Although our modeling parameter, f sed , aims to self-consistently capture these processes in a tractable way, the global properties of each individual object must ultimately define the true properties of the clouds.…”
Section: The Modelsmentioning
confidence: 99%
“…We consider example atmospheres ( Figure 1) using the Drift-Phoenix model atmosphere and cloud formation code (Hauschildt & Baron 1999;Helling et al 2004Helling et al , 2008bHelling & Woitke 2006;Dehn 2007;Witte et al 2009Witte et al , 2011 characterised by T eff = 1500 K and T eff = 2400 K, for both log g = 3.0 and log g = 5.0; and solar metallicities ([M/H]=0.0). These example atmospheres cover a wide and inclusive range of parameter space.…”
Section: Resultsmentioning
confidence: 99%