Dynamic Meteorology at the Photosphere of HD 209458b

By Curtis S. Cooper, A. Showman. 2005

193 citations recorded by the source corpus.

We calculate the meteorology of the close-in transiting extrasolar planet HD 209458b using a global, three-dimensional atmospheric circulation model. Dynamics are driven by perpetual irradiation of one hemisphere of this tidally locked planet. The simulation predicts global temperature contrasts of ~500 K at the photosphere and the development of a steady superrotating jet. The jet extends from the equator to midlatitudes and from the top model layer at 1 mbar down to 10 bar at the base of the heated region. Wind velocities near the equator exceed 4 km s-1 at 300 mbar. The hottest regions of the atmosphere are blown downstream from the substellar point by ~60° of longitude. We predict from these results a factor of ~2 ratio between the maximum and minimum observed radiation from the planet over a full orbital period, with peak infrared emission preceding the time of the secondary eclipse by ~14 hr.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/e7517ef8d895512684a72a773ea112301add17b1

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In Astronomy and Astrophysics

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

Citations in the corpus

• EQUATORIAL SUPERROTATION ON TIDALLY LOCKED EXOPLANETS (2011, methodology): “…zero-eccentricity hot Jupiters exhibit relatively steady circulation patterns whose velocity and temperature patterns are approximately symmetric about the equator (Showman & Guillot 2002; Cooper & Showman 2005, 2006; Showman et al. 2008, 2009; DobbsDixon & Lin 2008; Rauscher & Menou 2010).”
• CAN TiO EXPLAIN THERMAL INVERSIONS IN THE UPPER ATMOSPHERES OF IRRADIATED GIANT PLANETS? (2009, background): “…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 & Lin 2008; Showman et al. 2008a;…”
• Hot nights on extrasolar planets: mid‐infrared phase variations of hot Jupiters (2007, background): “Cooper & Showman (2005, 2006) determine energy recirculation and predict global temperature contrasts of ∼500 K at the photosphere.”
• TRANSMISSION SPECTRA OF THREE-DIMENSIONAL HOT JUPITER MODEL ATMOSPHERES (2009, methodology): “…dynamics using highly idealized prescriptions for the trmodynamic heating/cooling rate, such as a Newtonian relaxation scheme (Showman & Guillot 2002; Cooper & Showman 2005, 2006; Showman et al. 2008; Menou & Rauscher 2009; Rauscher & Menou 2009) or flux-limited diffusion (Dobbs-Dixon & Lin 2008).”
• 3D mixing in hot Jupiters atmospheres. I. Application to the day/night cold trap in HD 209458b (2013, background): “…circulation patterns including both strong horizntal and vertical velocities that are necessary for mixing tohappen (e.g., Showman & Guillot 2002; Cooper & Showman 2005, 2006; Showman et al. 2008, 2013; Rauscher & Menou 2012b,a, 2013; Heng et al. 2011a,b, 2012; Lewis et al. 2010; DobbsDixon &…”
• THE CLIMATE OF HD 189733b FROM FOURTEEN TRANSITS AND ECLIPSES MEASURED BY SPITZER (2010, background): “This was predicted by Cooper and Showman (2005), and is attributed to the advection of energy by a super-rotating wind encircling the equator of the planet.”
• Dynamics and Disequilibrium Carbon Chemistry in Hot Jupiter Atmospheres, with Application to HD 209458b (2006, methodology): “Despite adjustments to the cooling scheme (see §4.4), the temperatures, wind speeds, and flow geometry of the nominal model are broadly consistent with simulations published by Cooper & Showman (2005).”
• ATMOSPHERIC CIRCULATION OF HOT JUPITERS: COUPLED RADIATIVE-DYNAMICAL GENERAL CIRCULATION MODEL SIMULATIONS OF HD 189733b and HD 209458b (2008, unknown): “Like earlier work with simplified forcing (Showman et al. 2008a; Cooper & Showman 2005; Showman & Guillot 2002), our simulations develop a broad eastward equatorial jet, mean westward flow at high latitudes, and substantial flow over the poles at low pressure.”
• Atmospheric circulation of tidally locked exoplanets: a suite of benchmark tests for dynamical solvers (2010, methodology): “Thermal forcing for a tidally locked (exo)planet can be mimicked by replacing the −sin 2 term in equation (15) with a term that is proportional to +cos ( − 180◦)cos (see e.g. Cooper & Showman 2005; Menou & Rauscher 2009; Merlis & Schneider 2010).”
• The Influence of Atmospheric Dynamics on the Infrared Spectra and Light Curves of Hot Jupiters (2006, methodology): “As discussed in Cooper & Showman (2005) and CS06, while these models all possess similarly strong east-to-west jets, the dynamicalatmospheres differ slightly in detail.”
• ATMOSPHERIC HEAT REDISTRIBUTION ON HOT JUPITERS (2013, unknown): “…this timescale compar- ison could describe the pressure-, opacity-, and insolationdependence of the day-night temperature differences on hot Jupiters (Cooper & Showman 2005; Showman et al. 2008; Fortney et al. 2008; Rauscher & Menou 2010; Heng et al. 2011; Cowan & Agol 2011; Perna et al. 2012).”
• A Unified Theory for the Atmospheres of the Hot and Very Hot Jupiters: Two Classes of Irradiated Atmospheres (2007, methodology): “Several km s−1 winds, which are similar to the sound speed, are in line with predictions of a number of 2D and 3D dynamical models for hot Jupiter atmospheres (Showman & Guillot 2002; Cooper & Showman 2005; Langton & Laughlin 2007; Dobbs-Dixon & Lin 2007).”
• INFERENCE OF INHOMOGENEOUS CLOUDS IN AN EXOPLANET ATMOSPHERE (2013, unknown): “…produced from a range of general circulation models for tidally-locked hot-Jupiters forced using various methods, including Newtonian cooling (e.g. Cooper & Showman 2005; Showman et al. 2008; Dobbs-Dixon et al. 2010; Rauscher & Menou 2010; Heng et al. 2011a), dual-band radiative transfer (e.g.…”
• Inverting Phase Functions to Map Exoplanets (2008, methodology): “Although it may be possible to glean useful information from the phase function light curves of planets with such variable atmospheres, we elect in this Letter to ignore time variability, in line with the detailed modeling of Cooper & Showman (2005).”
• Atmospheric Circulation of Hot Jupiters: Three-dimensional Circulation Models of HD 209458b and HD 189733b with Simplified Forcing (2008, unknown): “Consistent with the results of Cooper & Showman (2005, 2006), the imposed day-night heating contrasts lead to rapid development of large day-night temperature differences and winds reaching several kmsec - 1 .”
• MULTIWAVELENGTH CONSTRAINTS ON THE DAY–NIGHT CIRCULATION PATTERNS OF HD 189733b (2008, background): “These same models indicate that the daynight temperature difference should increase with altitude (Cooper & Showman 2005; Showman et al. 2008; Dobbs-Dixon & Lin 2008), but this change is modest over the factor of 2−3 variation in the pressures that are likely sensed by these two bandpasses.”