The Changing Face of the Extrasolar Giant Planet HD 209458b

By J. Cho, Kristen Menou, Brad M. S. Hansen, Sara Seager. 2002

162 citations recorded by the source corpus.

High-resolution atmospheric flow simulations of the tidally locked extrasolar giant planet HD 209458b show large-scale spatio-temporal variability. This is in contrast to the simple, permanent day/night (i.e., hot/cold) picture. The planet's global circulation is characterized by a polar vortex in motion around each pole and a banded structure corresponding to approximately three broad zonal (east-west) jets. For very strong jets, the circulation-induced temperature difference between moving hot and cold regions can reach up to ~1000 K, suggesting that atmospheric variability could be observed in the planet's spectral and photometric signatures.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/0846dc4dcaff98e100ca60d8892fd8780019a25a

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In Astronomy and Astrophysics

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

Citations in the corpus

• ATMOSPHERIC CIRCULATION OF HOT JUPITERS: COUPLED RADIATIVE-DYNAMICAL GENERAL CIRCULATION MODEL SIMULATIONS OF HD 189733b and HD 209458b (2008, unknown): “Several groups have investigated a range of 2D and 3D models (Showman & Guillot 2002; Cho et al. 2003, 2008; Cooper & Showman 2005, 2006; Showman et al. 2008a,b; Langton & Laughlin 2007, 2008; Dobbs-Dixon & Lin 2008).”
• MULTIWAVELENGTH CONSTRAINTS ON THE DAY–NIGHT CIRCULATION PATTERNS OF HD 189733b (2008, background): “This assumes that the planet does not experience significant weather-related variability, such as that suggested by Cho et al. (2003, 2008) and Rauscher et al. (2008).”
• Possible Solutions to the Radius Anomalies of Transiting Giant Planets (2006, background): “A number of groups are attempting to address this issue with multidimensional, although approximate, numerical tools (Menou et al. 2003; Cho et al. 2003; Burkert et al. 2005; Cooper & Showman 2005), but these efforts are only in their early stages.”
• Atmospheric Loss of Exoplanets Resulting from Stellar X-Ray and Extreme-Ultraviolet Heating (2003, background): “The value ofa may be reduced close to by the action of strong14 thermospheric winds expected at close orbital distances (e.g., Cho et al. 2003).”
• Sodium Absorption from the Exoplanetary Atmosphere of HD 189733b Detected in the Optical Transmission Spectrum (2007, background): “…feature appears to be significantly blueshifted from the stellar line center, by ∼38 km s−1, and may be a combination of the planetary orbital motion and high speed winds flowing from the hot dayside, predicted by several dynamical atmospheric models (e.g., Cho et al. 2003; Cooper & Showman 2005).”
• Phase-dependent Properties of Extrasolar Planet Atmospheres (2005, background): “…motion on EGP atmospheres have been modeled by a variety of groups, each predicting some level of atmospheric circulation that depends strongly on adopted opacities and general approaches to the problem (Showman & Guillot 2002; Cho et al. 2003; Burkert et al. 2005; Cooper & Showman 2005).”
• The effect of condensates on the characterization of transiting planet atmospheres with transmission spectroscopy (2005, background): “It is certainly possible that this condition will not be met in reality (see Showman & Guillot 2002; Cho et al. 2003; Cooper & Showman 2005; Barman et al. 2005).”
• ATMOSPHERIC HEAT REDISTRIBUTION ON HOT JUPITERS (2013, unknown): “Simplified models have therefore played an important role in atmospheric dynamics of giant planets, both solar (Dowling & Ingersoll 1989; Cho & Polvani 1996; Scott & Polvani 2007; Showman 2007) and extrasolar (Cho et al. 2003, 2008; Showman & Polvani 2011; Showman et al. 2013a).”
• Atmospheric circulation of tidally locked exoplanets: a suite of benchmark tests for dynamical solvers (2010, methodology): “…describe the atmospheric dynamics, its radiative transfer, as well as – in principle – the chemistry and the cloud physics (Showman & Guillot 2002; Cho et al. 2003, 2008; Cooper & Showman 2005, 2006; Langton & Laughlin 2008; Menou & Rauscher 2009; Showman et al. 2009; Burrows et al. 2010;…”
• The Influence of Atmospheric Dynamics on the Infrared Spectra and Light Curves of Hot Jupiters (2006, background): “…past few years, several groups have computed dynamical atmosphere models for HD 209458b in an effort to understand the structure, winds, and temperature contrasts of the planet’s atmosphere (Showman & Guillot 2002; Cho et al. 2003; Cooper & Showman 2005; Burkert et al. 2005; Cooper & Showman 2006).”
• Comparative Planetary Atmospheres: Models of TrES-1 and HD 209458b (2005, background): “Atmospheric dynamics will redistribute this absorbed energy around the planet with an efficiency that is currently unknown (Showman & Guillot 2002; Cho et al. 2003; Burkert et al. 2005; Cooper & Showman 2005).”
• CAN TiO EXPLAIN THERMAL INVERSIONS IN THE UPPER ATMOSPHERES OF IRRADIATED GIANT PLANETS? (2009, background): “…lead to large temperature differences and powerful winds, as has been predicted by atmospheric general circulation models (GCMs) (Showman & Guillot 2002; Cho et al. 2003; Menou et al. 2003; Cooper & Showman 2005; Burkert et al. 2005; Langton & Laughlin 2007, 2008b,a; Cho et al. 2008; Dobbs-Dixon &…”
• Inverting Phase Functions to Map Exoplanets (2008, methodology): “The insensitivity of phase functions to the first and most important odd mode, j = 3, leads to ∼ 10% errors in the resulting map, based on the maps of Cho et al. (2003) and Showman et al. (2008).”
• A time-dependent radiative model of HD 209458b (2004, methodology): “On the other hand, the fact that Cho et al. (2003) obtain temperatures on the night side that can be hotter than on the day side is difficult to explain in light of our results.”
• Dynamic Meteorology at the Photosphere of HD 209458b (2005, background): “Preliminary simulations of the circulation by Showman & Guillot (2002) and the shallow-water calculations of Cho et al. (2003) suggest that close-in systems like HD 209458b—with strong daynight heating contrasts and modest rotation rates—occupy a dynamically interesting regime.”