2003
DOI: 10.1086/377080
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Abstract: We show that under certain circumstances the differences between the absorption mean and Planck mean opacities can lead to multiple solutions for an LTE atmospheric structure. Since the absorption and Planck mean opacities are not expected to differ significantly in the usual case of radiative equilibrium, non-irradiated atmospheres, the most interesting situations where the effect may play a role are strongly irradiated stars and planets, and also possibly structures where there is a significant deposition of… Show more

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Cited by 433 publications
(530 citation statements)
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References 27 publications
(32 reference statements)
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“…Following Mihalas (1978) (see also Hubeny et al 2003), I define three moments of the specific intensity as:…”
Section: Settingmentioning
confidence: 99%
See 1 more Smart Citation
“…Following Mihalas (1978) (see also Hubeny et al 2003), I define three moments of the specific intensity as:…”
Section: Settingmentioning
confidence: 99%
“…Note that this approach is valid in two extreme cases: for isotropic irradiation (e.g. Hubeny et al 2003), for which μ * = 1/ √ 3, or in the case of collimated visible irradiation (e.g. Meador & Weaver 1980), in which case μ * = cos θ * .…”
Section: The Incoming (Visible) Radiationmentioning
confidence: 99%
“…Equilibrium chemistry abundances, 248 Jonathan J. Fortney the depth to which incident flux will penetrate into a planet's atmosphere, and the radiative time constant as a function of pressure and temperature in the atmosphere all naturally define two classes these irradiated planets. Those planets that are warmer than required for condensation of titanium (Ti) and vanadium (V)-bearing compounds will possess a temperature inversion at low pressure due to absorption of incident flux by TiO and VO (a hot stratosphere, as first found by Hubeny et al 2003), and will appear "anomalously" bright in secondary eclipse at mid-infrared wavelengths. Furthermore, these planets will have large day/night effective temperature contrasts and their optical flux will be dominated by thermal emission.…”
Section: Introductionmentioning
confidence: 99%
“…We note that the 1σ error bars on the stellar T eff s and radii could actually lead to a 10% difference in incident flux between them. Also, planetary atmospheric metallicity could play a role, especially for the temperatures for condensation of Ti and V. At the modest temperatures of XO-1b, TiO/VO can probably only be found at the substellar point (where it is hottest), if the molecules make it above a possible cold trap (Hubeny et al 2003). Perhaps only VO is present, rather than TiO, since V condenses more gradually with reduced temperature (Lodders 2002).…”
mentioning
confidence: 99%
“…See also [30,26,27,28]. Hot planets such as Ups And are on one side of a temperature-driven chemical composition boundary, while cooler planets such as HD 209458b are on the cooler side.…”
Section: Figmentioning
confidence: 99%