Atmospheric circulation and tides of ``51 Pegasus b-like'' planets

By A. Showman, T. Guillot. 2002

522 citations recorded by the source corpus.

We examine the properties of the atmospheres of extrasolar giant planets at orbital distances smaller than 0.1 AU from their stars. We show that these \51 Peg b-like" planets are rapidly synchronized by tidal in- teractions, but that small departures from synchronous rotation can occur because of fluid-dynamical torques within these planets. Previous radiative-transfer and evolution models of such planets assume a homogeneous atmosphere. Nevertheless, we show using simple arguments that, at the photosphere, the day-night temperature dierence and characteristic wind speeds may reach500 K, and 2k m s 1 , respectively. Substantial departures from chemical equilibrium are expected. The cloud coverage depends sensitively on the dynamics; clouds could exist predominantly either on the dayside or nightside, depending on the circulation regime. Radiative-transfer models that assume homogeneous conditions are therefore inadequate in describing the atmospheric properties of 51 Peg b-like planets. We present preliminary three-dimensional, nonlinear simulations of the atmospheric cir- culation of HD 209458b that indicate plausible patterns for the circulation and generally agree with our simpler estimates. Furthermore, we show that kinetic energy production in the atmosphere can lead to the deposition of substantial energy in the interior, with crucial consequences for the evolution of these planets. Future measure- ments of reflected and thermally-emitted radiation from these planets will help test our ideas.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/5d2c65e7426584610e850c6738ed0385b5431e2b

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In Astronomy and Astrophysics

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

Citations in the corpus

• TRANSMISSION SPECTRA OF THREE-DIMENSIONAL HOT JUPITER MODEL ATMOSPHERES (2009, methodology): “…have forced the 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…”
• Predicting low-frequency radio fluxes of known extrasolar planets (2007, background): “Thermal atmospheric tides resulting from stellar heating can drive planets away from synchronous rotation (Showman & Guillot, 2002; Correia et al., 2003; Laskar & Correia, 2004).”
• ROTATION AND WINDS OF EXOPLANET HD 189733 b MEASURED WITH HIGH-DISPERSION TRANSMISSION SPECTROSCOPY (2015, background): “Finally, the atmosphere and the planet interior do not always reach perfect tidal synchronization (Showman & Guillot 2002), meaning that global atmospheric superrotation or sub-rotation are also possible.”
• From thermal dissociation to condensation in the atmospheres of ultra hot Jupiters: WASP-121b in context (2018, background): “In the re- gions dominated by H instead of H2, Cp should be twice as big, µ twice as small, and γ should become equal to 1+2/3 (Showman & Guillot 2002).”
• Characterization of exoplanets from their formation - I. Models of combined planet formation and evolution (2012, background): “…several possible physical mechanisms leading to this bloating, such as tidal heating (Bodenheimer et al. 2001), dissipation of stellar irradiation deep in the interior (Showman & Guillot 2002), ohmic dissipation (Batygin & Stevenson 2010), and double diffusive convection (Chabrier & Baraffe 2007).”
• 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).”
• A time-dependent radiative model of HD 209458b (2004, methodology): “We compute the temperature profiles for rotation periods corresponding to equatorial wind velocities of 0.5, 1 and 2 km s−1, in the range predicted by Showman & Guillot (2002).”
• THE MASS OF KOI-94d AND A RELATION FOR PLANET RADIUS, MASS, AND INCIDENT FLUX (2013, background): “These mechanisms are discussed in a variety of papers: weather layer kinetic energy transport (Showman & Guillot 2002; Guillot & Showman 2002), Ohmic dissipation (Batygin & Stevenson 2010; Perna et al. 2010), thermal tides (Arras & Socrates 2010), and mechanical greenhouse (Youdin & Mitchell 2010).”
• CAN TiO EXPLAIN THERMAL INVERSIONS IN THE UPPER ATMOSPHERES OF IRRADIATED GIANT PLANETS? (2009, background): “…rotating planets can 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…”
• MULTIWAVELENGTH CONSTRAINTS ON THE DAY–NIGHT CIRCULATION PATTERNS OF HD 189733b (2008, background): “…models predict that the regions of maximum and minimum flux will be shifted to the east of the substellar and antistellar points, respectively, by amounts analogous to that suggested by our flux maps (Showman & Guillot 2002; Cooper & Showman 2005; Fortney et al. 2006b; Showman et al. 2008).”
• WASP-121 b: a hot Jupiter close to tidal disruption transiting an active F star (2015, background): “…(Bodenheimer et al. 2001), deposition of kinetic energy into the planets from strong winds driven by the large day/night temperature contrasts (Showman & Guillot 2002), enhanced atmospheric opacities (Burrows et al. 2007), reduced heat transport efficiency by layered convection inside the…”
• 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.”
• The Effect of Tidal Inflation Instability on the Mass and Dynamical Evolution of Extrasolar Planets with Ultrashort Periods (2003, background): “But, the resulting longitudinal pressure gradient would excite large scale circulation with speeds comparable to cs of the hot side (Showman & Guillot 2002, Burkert et al. 2002); it is not clear yet what the resulting temperature on the dark side would be.”
• Atmospheric Circulation of Hot Jupiters: Three-dimensional Circulation Models of HD 209458b and HD 189733b with Simplified Forcing (2008, unknown): “Cooper & Showman (2005, 2006) and Showman & Guillot (2002) focused on HD209458b and approximated the day-side heating and nightside cooling using a Newtonian cooling/heating scheme, which parameterizes the radiative heating rate (in Ksec - 1 ) as ( T eq T ) /τ rad , where T eq is the speci-fied…”
• Atmospheric circulation of tidally locked exoplanets: a suite of benchmark tests for dynamical solvers (2010, background): “…Cho & Menou 2010), which 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;…”
• ATMOSPHERIC HEAT REDISTRIBUTION ON HOT JUPITERS (2013, unknown): “Showman & Guillot (2002) first suggested that hot Jupiters will exhibit large fractional dynight temperature differences whenτrad ≪ τadv and small fractional day-night temperature differences whenτrad ≫ τadv.”