Theoretical Spectra and Atmospheres of Extrasolar Giant Planets

By D. Sudarsky, Adam Burrows, I. Hubeny. 2002

267 citations recorded by the source corpus.

We present a comprehensive theory of the spectra and atmospheres of irradiated extrasolar giant planets. We explore the dependences on stellar type, orbital distance, cloud characteristics, planet mass, and surface gravity. Phase-averaged spectra for specific known extrasolar giant planets that span a wide range of the relevant parameters are calculated, plotted, and discussed. The connection between atmospheric composition and emergent spectrum is explored in detail. Furthermore, we calculate the effect of stellar insolation on brown dwarfs. We review a variety of representative observational techniques and programs for their potential for direct detection, in light of our theoretical expectations, and we calculate planet-to-star flux ratios as a function of wavelength. Our results suggest which spectral features are most diagnostic of giant planet atmospheres and reveal the best bands in which to image planets of whatever physical and orbital characteristics.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/7ef1edc528629ae3ea202007d60ddf387e10066c

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Citations in the corpus

Planetary Radii across Five Orders of Magnitude in Mass and Stellar Insolation: Application to Transits (2006, background): “…At Gyr ages, we find Bond albedos of∼0.05-0.1 at distances less than 0.1 AU, and higher values of∼0.3-0.4 from 1-10 AU, where cooler temperatures prevail andso ium and potassium, which absorb strongly in the optical, have condensed into clouds below the visible atmosphere (Sudarsky et al. 2003).”
HST hot-Jupiter transmission spectral survey: detection of potassium in WASP-31b along with a cloud deck and Rayleigh scattering (2014, background): “…models of hot Jupiters have predominately predicted atmospheres which are dominated by water opacity in the near-IR, with the optical containing alkali features and scattering by hydrogen molecules (e.g. Seager & Sasselov 2000; Sudarsky et al. 2003; Burrows et al. 2010; Fortney et al. 2010).”
Comparative Planetary Atmospheres: Models of TrES-1 and HD 209458b (2005, result): “While a number of papers have aimed at predicting the optical and infrared spectra of hot EGPs (Seager & Sasselov 1998; Marley et al. 1999; Barman et al. 2001; Sudarsky et al. 2003), these results are the first infrared detections (rather than upper limits) that can be compared with models.”
A variationally computed line list for hot NH3 (2010, background): “These temperature and pressure dependencies suggest that the outer atmospheres of extrasolar giant planets at large orbital distances will contain significant quantities of ammonia (Sudarsky et al. 2003), and it is likely that NH3 will soon be confirmed to be present in these objects.”
THE IMPRINT OF EXOPLANET FORMATION HISTORY ON OBSERVABLE PRESENT-DAY SPECTRA OF HOT JUPITERS (2016, background): “The resulting effect of such small differences in log(g) on planetary emission spectra of hot Jupiters are very small (Sudarsky et al. 2003; Mollière et al. 2015) and the internal thermodynamic evolution for hot Jupiters is much less important for the spectral shape than the SED and strength of…”
Dynamics and Disequilibrium Carbon Chemistry in Hot Jupiter Atmospheres, with Application to HD 209458b (2006, background): “It should be noted, however, that the CO null detection reported by Deming et al. (2005a) relies on the radiative-equilibrium calculations of Sudarsky et al. (2003).”
C/O RATIO AS A DIMENSION FOR CHARACTERIZING EXOPLANETARY ATMOSPHERES (2012, background): “…typically assumed solar abundances and chemical equilibrium in models of exoplanetary atmospheres and focused primarily on characterizing hot Jupiters based on their temperature structures (Seager & Sasselov 1998; Sudarsky et al. 2003; Hubeny et al. 2003; Barman et al. 2005; Fortney et al. 2008).”
THE STATISTICS OF ALBEDO AND HEAT RECIRCULATION ON HOT EXOPLANETS (2009, background): “They are all Class IV and V extrasolar giant planets in the scheme of Sudarsky et al. (2003).”
Aeronomy of extra-solar giant planets at small orbital distances (2003, background): “Numerous studies of the lower atmospheres of EGPs have carried out (cf.Sudarsky et al., 2003, and references therein E-mail address: yelle@lpl.arizona.edu.”
The effect of condensates on the characterization of transiting planet atmospheres with transmission spectroscopy (2005, methodology): “In addition, Fortney et al. (2003) utilized a different model atmosphere program (see Sudarsky et al. 2003).”
A correlation between the heavy element content of transiting extrasolar planets and the metallicity of their parent stars (2006, methodology): “…as the difference between the measured radius and the one calculated using a simple evolution model for a solar composition gaseous planet. temperatures in the literature can vary by up to 500 K (Barman et al. 2001; Sudarsky et al. 2003; Fortney et al. 2005; Iro et al. 2005; Seager et al. 2005).”
The 3.6-8.0 μm Broadband Emission Spectrum of HD 209458b: Evidence for an Atmospheric Temperature Inversion (2007, result): “…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).”
TRANSMISSION SPECTRA OF THREE-DIMENSIONAL HOT JUPITER MODEL ATMOSPHERES (2009, background): “Other authors have previously explored reflection and emission spectra (e.g. Marley et al. 1999; Sudarsky et al. 2000; Barman et al. 2001; Sudarsky et al. 2003; Marley et al. 2007), but here we briefly examine transmission spectra for these atmospheres.”