Comparative Planetary Atmospheres: Models of TrES-1 and HD 209458b

By Jon Fortney, M. Marley, K. Lodders, D. Saumon, R. Freedman. 2005

224 citations recorded by the source corpus.

We present new self-consistent atmosphere models for the transiting planets TrES-1 and HD 209458b. The planets were recently observed with the Spitzer Space Telescope in bands centered on 4.5 and 8.0 μm, for TrES-1, and 24 μm, for HD 209458b. We find that standard solar-metallicity models fit the observations for HD 209458b. For TrES-1, which has a Teff ~300 K cooler, we find that models with a metallicity 3-5 times enhanced over solar abundances can match the 1 σ error bar at 4.5 μm and 2 σ at 8.0 μm. Models with solar abundances that include energy deposition into the stratosphere give fluxes that fall within the 2 σ error bars in both bands. The best-fit models for both planets assume that reradiation of absorbed stellar flux occurs over the entire planet. For all models of both planets, we predict planet-to-star flux ratios in other Spitzer bandpasses.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/dab100b539ee49192d0a70b1ce4d4450dc0d4a82

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In Astronomy and Astrophysics

1. Jon Fortney
2. N. Madhusudhan
3. A. Showman
4. M. Marley
5. Sara Seager
6. H. Knutson
7. D. Charbonneau
8. D. Deming

Citations in the corpus

• INFERENCE OF INHOMOGENEOUS CLOUDS IN AN EXOPLANET ATMOSPHERE (2013, methodology): “We use the methods of Fortney et al. (2005, 2008) to compute Kepler-7b’s one-dimensional (1D) temperature structure and emission spectrum (Fig.5).”
• The effect of condensates on the characterization of transiting planet atmospheres with transmission spectroscopy (2005, background): “For TrES-1, which although similar in mass has a 30% smaller radius and is ∼ 300 K colder in effective temperature (Fortney et al. 2005), we find η = 50.”
• Theoretical Spectral Models of the Planet HD 209458b with a Thermal Inversion and Water Emission Bands (2007, background): “…low upper limit of Richardson, Deming, & Seager (2003) in the K band that was problematic in the previous theory (Burrows, Hubeny, & Sudarsky 2005; Fortney et al. 2005; Barman, Hauschildt, & Allard 2005) is comfortably consistent with the models with an extra upper-atmosphere absorber in the…”
• QUANTITATIVELY ASSESSING THE ROLE OF CLOUDS IN THE TRANSMISSION SPECTRUM OF GJ 1214b (2013, background): “…planets and moons, brown dwarfs, and exoplanets, with both cloudy and clear atmospheres; the models are described in McKay et al. (1989); Marley et al. (1996); Burrows et al. (1997); Marley & McKay (1999); Marley et al. (2002); Fortney et al. (2005); Saumon & Marley (2008); Fortney et al. (2008).”
• Planetary Radii across Five Orders of Magnitude in Mass and Stellar Insolation: Application to Transits (2006, unknown): “…study of giant planet thermal structure by Marley & McKay (1999) and has also been employed to study the atmospheres of the hot Jupiters (Marley 1998; Fortney et al. 2005, 2006) as well as brown dwarfs (Marley et al. 1996; Burrows et al. 1997; Marley et al. 2002), albeit without incident radiation.”
• A SYSTEMATIC RETRIEVAL ANALYSIS OF SECONDARY ECLIPSE SPECTRA. II. A UNIFORM ANALYSIS OF NINE PLANETS AND THEIR C TO O RATIOS (2013, methodology): “Furthermore, Fortney et al. (2005) suggested that many cloud species (minor condensates and photochemical hazes) will have small normal optical depths resulting in minimal impact on emission spectra.”
• A Unified Theory for the Atmospheres of the Hot and Very Hot Jupiters: Two Classes of Irradiated Atmospheres (2007, background): “However, in our past work we have found only weak effects onP-T profiles and spectra due to cloud opacity (Fortney et al. 2005), so we ignore cloud opacity here.”
• GASEOUS MEAN OPACITIES FOR GIANT PLANET AND ULTRACOOL DWARF ATMOSPHERES OVER A RANGE OF METALLICITIES AND TEMPERATURES (2014, background): “…et al. (2008) (hereafter, F08) we presented a detailed discussion of atomic and molecular line opacities used by our group in modeling the atmospheres of brown dwarfs and giant planets (e.g. Marley et al. 2002; Fortney et al. 2005; Saumon & Marley 2008; Fortney et al. 2008; Marley et al. 2010).”
• EXOPLANET ALBEDO SPECTRA AND COLORS AS A FUNCTION OF PLANET PHASE, SEPARATION, AND METALLICITY (2010, methodology): “D iterative radiative-convective atmo- sphere model previously used in Marley (1997); Burrows et al. (1997); Marley et al. (1999a, 2002); Fortney et al. (2005, 2006, 2007); Fortney & Marley (2007) and Fortney et al. (2008a,b).”
• Atmospheric Circulation of Hot Jupiters: Three-dimensional Circulation Models of HD 209458b and HD 189733b with Simplified Forcing (2008, unknown): “…plane-parallel multi-stream radiative transfer code first used for Titan by McKay et al. (1989) and later extended to giant planets and brown dwarfs by Marley, Fortney, and collaborators (Marley et al. 1996; Burrows et al. 1997; Marley & McKay 1999; Marley et al. 1999; Fortney et al. 2005, 2006b,a).”
• WATER VAPOR IN THE SPECTRUM OF THE EXTRASOLAR PLANET HD 189733b. I. THE TRANSIT (2014, methodology): “Fortney et al. (2005) and Morley et al. (2013) show the condensation curves of various species in pressure-temperature phase space.”
• The 3.6-8.0 μm Broadband Emission Spectrum of HD 209458b: Evidence for an Atmospheric Temperature Inversion (2007, background): “…the dayside emission spectra for the non-inflated hot Jupiters (excluding the core-dominated HD 149026b) are broadly consistent with the predictions of standard cloud-free atmosphere models (Sudarsky et al. 2003; Seager et al. 2005; Barman et al. 2005; Fortney et al. 2005; Burrows et al. 2006).”
• Atmosphere, Interior, and Evolution of the Metal-rich Transiting Planet HD 149026b (2005, methodology): “It was significantly revised to model the atmospheres of brown dwarfs (Marley et al. 1996; Burrows et al. 1997; Marley et al. 2002), Uranus (Marley & McKay 1999), cool EGPs (Marley 1998), and Pegasi planets (Fortney et al. 2005).”
• C/O RATIO AS A DIMENSION FOR CHARACTERIZING EXOPLANETARY ATMOSPHERES (2012, background): “…possible only recently (Madhusudhan et al. 2011a), nominal constraints on atmospheric C, O, and/or C/O have been reported for several transiting exoplanets in the past decade (e.g. Fortney et al. 2005; Seager et al. 2005; Madhusudhan & Seager 2009,2010,2011; Desert et al. 2009; Swain et al. 2009).”
• The TRAPPIST survey of southern transiting planets. I. Thirty eclipses of the ultra-short period planet WASP-43 b (2012, methodology): “We have modeled the atmosphere of WASP-43 b using the methods described in Fortney et al. (2005, 2008) and Fortney & Marley (2007).”
• The Very Low Albedo of an Extrasolar Planet: MOST Space-based Photometry of HD 209458 (2007, methodology): “Atmospheric models by Fortney et al. (2005) predict an effective temperature of 1442 K, assuming 4 reradiation and solar metallicity.”
• Infrared Transmission Spectra for Extrasolar Giant Planets (2006, methodology): “DISCUSSION In our model we did not include the contribution of hazes or clouds (Ackerman & Marley 2001; Lunine et al. 1989; Fortney et al. 2005).”