TRANSMISSION SPECTRA OF THREE-DIMENSIONAL HOT JUPITER MODEL ATMOSPHERES

By Jon Fortney, M. Shabram, A. Showman, Y. Lian, R. Freedman, M. Marley, N. Lewis. 2009

218 citations recorded by the source corpus.

We compute models of the transmission spectra of planets HD 209458b, HD 189733b, and generic hot Jupiters. We examine the effects of temperature, surface gravity, and metallicity for the generic planets as a guide to understanding transmission spectra in general. We find that carbon dioxide absorption at 4.4 and 15 μm is prominent at high metallicity, and is a clear metallicity indicator. For HD 209458b and HD 189733b, we compute spectra for both one-dimensional and three-dimensional model atmospheres and examine the differences between them. The differences are usually small, but can be large if atmospheric temperatures are near important chemical abundance boundaries. The calculations for the three-dimensional atmospheres, and their comparison with data, serve as constraints on these dynamical models that complement the secondary eclipse and light curve data sets. For HD 209458b, even if TiO and VO gases are abundant on the dayside, their abundances can be considerably reduced on the cooler planetary limb. However, given the predicted limb temperatures and TiO abundances, the model's optical opacity is too high. For HD 189733b we find a good match with some infrared data sets and constrain the altitude of a postulated haze layer. For this planet, substantial differences can exist between the transmission spectra of the leading and trailing hemispheres, which are an excellent probe of carbon chemistry. In thermochemical equilibrium, the cooler leading hemisphere is methane-dominated, and the hotter trailing hemisphere is CO-dominated, but these differences may be eliminated by non-equilibrium chemistry due to vertical mixing. It may be possible to constrain the carbon chemistry of this planet, and its spatial variation, with James Webb Space Telescope.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/126d856dc5977b9d21f9a104d2402f5e2a5643d9

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In Astronomy and Astrophysics

1. N. Madhusudhan
2. Jon Fortney
3. A. Showman
4. D. Sing
5. D. Deming
6. M. Line
7. M. Marley
8. V. Parmentier

In Instrumentation

1. N. Madhusudhan
2. Jon Fortney
3. A. Showman
4. D. Sing
5. M. Line
6. H. Knutson
7. M. Marley
8. V. Parmentier

Citations in the corpus

• INFLATING HOT JUPITERS WITH OHMIC DISSIPATION (2010, methodology): “In our models, we adopt atmospheric temperature profiles similar to that of Spiegel et al. (2009) for HD209458b and Tres-4b, and the 1D profile of Fortney et al. (2010) for HD189733b.”
• HST PanCET Program: A Cloudy Atmosphere for the Promising JWST Target WASP-101b (2017, methodology): “We test the measured transmission spectrum against a suite of isothermal models calculated from a grid formulated in Fortney et al. (2010).”
• THE INFLUENCE OF NONUNIFORM CLOUD COVER ON TRANSIT TRANSMISSION SPECTRA (2015, methodology): “To date, only one-dimensional, limb averaged cloud models have been used to interpret the transmission spectra of exoplanets (Fortney et al. 2010; Howe & Burrows 2012; Morley et al. 2013;15; Kriedberg et al. 2014a;15; Fraine et al. 2014; Benneke 2015).”
• DISEQUILIBRIUM CARBON, OXYGEN, AND NITROGEN CHEMISTRY IN THE ATMOSPHERES OF HD 189733b AND HD 209458b (2011, methodology): “D “4pi” profile from Fortney et al. (2006a, 2010) is the coolest of all our models at 10-30 bars, resulting in the largest quenched HCN mole fraction in this model.”
• HST hot-Jupiter transmission spectral survey: detection of potassium in WASP-31b along with a cloud deck and Rayleigh scattering (2014, methodology): “We compare these spectral features to both analytic models and those from the modelling suites of Burrows et al. (2010) and Fortney et al. (2010).”
• A FRAMEWORK FOR CHARACTERIZING THE ATMOSPHERES OF LOW-MASS LOW-DENSITY TRANSITING PLANETS (2013, methodology): “The code we use to model transmission spectra is fully described in Hubbard et al. (2001), Fortney et al. (2010), and Shabram et al. (2011).”
• THERMAL PHASE VARIATIONS OF WASP-12b: DEFYING PREDICTIONS (2011, unknown): “Based on observations and models of HD 189733b (Fortney et al. 2010), one might therefore expect the transit depth at 4.5 μ m to be ∼ 10 − 3 deeper than at 3.6 μ m.”
• A DETECTION OF WATER IN THE TRANSMISSION SPECTRUM OF THE HOT JUPITER WASP-12b AND IMPLICATIONS FOR ITS ATMOSPHERIC COMPOSITION (2015, background): “However, theoretical models predict that most of the stellar radiation is attenuated in a fairly localized region within a few degrees of the terminator (Fortney et al. 2010).”
• Optimal estimation retrievals of the atmospheric structure and composition of HD 189733b from secondary eclipse spectroscopy (2011, background): “A spectral feature at 4.5µm can be explained by either of the carbon bearing molecules CO2 or CO, although it is still unclear which due to the degeneracy of the solution (Désert et al. 2009; Fortney et al. 2010).”
• JUPITER MODELS WITH IMPROVED AB INITIO HYDROGEN EQUATION OF STATE (H-REOS.2) (2011, background): “…disrupted (WASP-12b; Li et al. 2010), that are thought to have formed by gravitational instability (HR 8799be; Baruteau et al. 2011), or that even allow to study non-equilibrium chemistry in irradiated atmospheres (HD 189733b; Fortney et al. 2010), have drawn some attention away from Jupiter.”
• An HST optical-to-near-IR transmission spectrum of the hot Jupiter WASP-19b: detection of atmospheric water and likely absence of TiO (2013, methodology): “For both data sets, we compare to two different sets of models; one set based on the formalism of Fortney et al. (2008, 2010) and the other set based on the formalism of Burrows et al. (2010) and Howe & Burrows (2012).”
• H2O abundances and cloud properties in ten hot giant exoplanets (2018, methodology): “The retrieval forward model has also been validated against results from radiative transfer codes of other groups (Fortney et al. 2010; Deming et al. 2013; Line et al. 2013; Heng & Kitzmann 2017), with which we find good agreement.”
• From thermal dissociation to condensation in the atmospheres of ultra hot Jupiters: WASP-121b in context (2018, methodology): “Despite this approximation, our method gives similar results for hot Jupiters to the more complex method used by Fortney et al. (2010).”
• The Complete Transmission Spectrum of WASP-39b with a Precise Water Constraint (2017, background): “…have greatly advanced our understanding of planetary systems, expanding theory and observations beyond our solar system (e.g. Seager & Deming 2010; Fortney et al. 2010; Marley et al. 2013; Deming et al. 2013; Stevenson et al. 2014; Sing et al. 2016; Kataria et al. 2016; Evans et al. 2016; Deming…”
• Transmission spectral properties of clouds for hot Jupiter exoplanets (2014, methodology): “The Fortney et al. (2010) model is a good fit to the optical slope, the 1.4 µm H2O feature, and the Spitzer data, though only contains an artificial pure-Rayleigh scattering component, which has no effect on the transmission spectrum longer than ∼2 µm.”
• Temperature–pressure profile of the hot Jupiter HD 189733b from HST sodium observations: detection of upper atmospheric heating (2012, background): “The models shown for comparison to HD 189733b are from Fortney et al. (2010), Yelle (2004) and Garćıa Muñoz (2007).”