Spectroscopy across the brown dwarf/planetary mass boundary - I. Near-infrared JHK spectra

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Volume 540 (April 2012)

A&A, 540 (2012) A85

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Table 4

Cloud models^a.

Physics	DUSTY	BT-Settl	Drift-PHOENIX	Gaia-Dusty	Marley et al.

Opacity source	30 dust species	43 dust species	7 dust species	updated DUSTY	5 dust species
Gas-dust phase^b	S = 1	S = 1.001	S = f(z,s)	S = 1	S = 1
Mixing	none	timescale from RHD	damping of turnover timescale	none	diffusive^c
Settling/Rainout	none	timescale comparison	equation of motion	none	parameterised in f_sed
Dust sizes	f(a) ∝ a^-3.5, (ISM)	timescale comparison	f(a,z)^d	f(a) ∝ a^-3.5, (ISM)	log-normal f(z,s)^e
	0.00625–0.24 μm	0.00625–0.24 μm	10^-6 − 100 μm	0.00625–0.24 μm	10^-5 − 1 μm
Chemistry	equilibrium	equilibrium	equilibrium^f	equilibrium^f	equilibrium except
					CO/CH₄, N₂/NH₃

Notes.

^(a)

PHOENIX (Hauschildt et al. 1999) DUSTY (Allard et al. 2001), BT-Settl (Allard et al. 2003, 2010), Drift-PHOENIX (Helling et al. 2008a; Witte et al. 2009), Gaia-Dusty (Rice et al. 2010), Marley et al. (Ackerman & Marley 2001; Marley et al. 2003; Saumon & Marley 2008; Freedman et al. 2008).

^(b)

S quantifies the supersaturation ratio. S = 1 for thermal equilibrium between the gas and dust.

^(c)

Parameterised in k_zz.

^(d)

f(a,z) is the grain size distribution at height z and provides the number of grains of size a.

^(e)

f(z,s) is the grain size distribution for a grain species s at height z.

^(f)

Updated chemistry treatment compared to DUSTY.

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