Evolution of "51 Pegasus b-like" planets

By T. Guillot, A. Showman. 2002

300 citations recorded by the source corpus.

About one-quarter of the extrasolar giant planets discovered so far have orbital distances smaller than 0.1 AU. These “51 Peg b-like” planets can now be directly characterized, as shown by the planet transiting in front the star HD 209458. We review the processes that affect their evolution. We apply our work to the case of HD 209458b, whose radius has been recently measured. We argue that its radius can be reproduced only when the deep atmosphere is assumed to be unrealistically hot. When using more realistic atmospheric temperatures, an energy source appears to be missing in order to explain HD 209458b's large size. The most likely source of energy available is not in the planet's spin or orbit, but in the intense radiation received from the parent star. We show that the radius of HD 209458b can be reproduced if a small fraction (~$1\%$) of the stellar flux is transformed into kinetic energy in the planetary atmosphere and subsequently converted to thermal energy by dynamical processes at pressures of tens of bars.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/541b688b180c474c5dbac3167a7898fade4aca3b

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In Astronomy and Astrophysics

1. Jon Fortney
2. D. Charbonneau
3. N. Madhusudhan
4. Sara Seager
5. M. Marley
6. C. Mordasini
7. J. Winn
8. A. Showman

Citations in the corpus

• Detection of Thermal Emission from an Extrasolar Planet (2005, background): “Of the various models for the inflated radius of a hot Jupiter (e.g., Bodenheimer et al. 2001; Guillot & Showman 2002; Burrows et al. 2003), the tidal dissipation of orbital eccentricity most naturally leads to a variety of observed planetary radii, since only some systems may contain additional…”
• On the Radii of Extrasolar Giant Planets (2003, methodology): “A planet with intermediate period will not be experiencing significant internal tidal dissipation but would still be irradiated to an extent sufficient to produce a significant amount of kinetic heating from the mechanism suggested by Guillot & Showman (2002).”
• The Interior Structure, Composition, and Evolution of Giant Planets (2009, background): “21 – Guillot & Showman (2002) proposed that a small fraction (∼0.5-1”
• Planetary Radii across Five Orders of Magnitude in Mass and Stellar Insolation: Application to Transits (2006, background): “The 14 transiting planets are all gas giants (See Guillot et al. 1996; Guillot & Showman 2002; Bodenheimer et al. 2003; Burrows et al. 2003; Baraffe et al. 2005; Laughlin et al. 2005; Arras & Bildsten 2006 for calculations of structure and contraction of many planets) although one planet, HD…”
• A time-dependent radiative model of HD 209458b (2004, methodology): “This mechanism thus cannot supply the energy source required at deep levels to explain the radius of HD 209458 (Guillot & Showman 2002; Baraffe et al. 2003).”
• THE MASS–METALLICITY RELATION FOR GIANT PLANETS (2015, background): “…planets (see, e.g., Guillot 2010for an analytic analysis, Spiegel & Burrows 2013for a review of the chemical and physical processes at play, and Guillot & Showman 2002for an application of a 2D boundary condition)and our uncertainty in where the heavy elements are within the planets (core…”
• ON THE ANOMALOUS RADII OF THE TRANSITING EXTRASOLAR PLANETS (2011, methodology): “…that there is a constant partitioning between thermal energy and kinetic energy, an assumption that conforms with the kinetic heating hypothesis of Guillot & Showman (2002), which posits that a fraction, η, of the total flux received by a planet is converted into kinetic energy by atmospheric…”
• THE HEAVY-ELEMENT MASSES OF EXTRASOLAR GIANT PLANETS, REVEALED (2011, background): “The reason for this effect has not been determined; a variety of additional internal energy sources or contraction-stalling mechanisms have been proposed (Guillot & Showman 2002; Jackson et al. 2009; Batygin et al. 2011; Chabrier & Baraffe 2007; Arras & Socrates 2010).”
• Transits and Occultations (2010, background): “…constituents that efficiently trap internal heat (Burrows et al. 2007); enhanced downward convection allowing the incident stellar radiation to reach significant depth (Guillot & Showman 2002); and inhibition of convection within the planet that raps internal heat (Chabrier & Baraffe 2007).”
• The Evolution of Gravitationally Unstable Protoplanetary Disks: Fragmentation and Possible Giant Planet Formation (2003, background): “In addition, for the transiting extrasolar giant HD 209458b, for which the planetary radius and mass are known (Charbonneau et al. 2000), models of the planet’s interior are generally consistent with the absence of a core (e.g., Guillot & Showman 2002).”
• The Gaia–Kepler Stellar Properties Catalog. II. Planet Radius Demographics as a Function of Stellar Mass and Age (2020, background): “…radius demographics, such as the hot sub-Neptunian desert (Lundkvist et al. 2016; Berger et al. 2018b; Dong et al. 2018), hot Jupiter inflation (Guillot & Showman 2002; Baraffe et al. 2010, 2014; Fortney & Nettelmann 2010; Laughlin & Lissauer 2015; Laughlin 2018; Komacek et al. 2020), and the…”
• The Transit Light Curve Project. I. Four Consecutive Transits of the Exoplanet XO-1b (2006, background): “In these models ∼ 2% of the stellar insolation is deposited at depth, following the work of Guillot & Showman (2002).”
• Atmosphere, Interior, and Evolution of the Metal-rich Transiting Planet HD 149026b (2005, background): “This has suggested to many that this one planet harbors an additional energy source that slows it contraction (Bodenheimer et al. 2001; Guillot & Showman 2002; Baraffe et al. 2003; Winn & Holman 2005).”
• HD 147506b: A Supermassive Planet in an Eccentric Orbit Transiting a Bright Star (2007, background): “…implying that it has a large heavy core (∼70M⊕; Laughlin et al. 2005), and several (HD 209458b, HAT-P-1b, WASP-1) have unexpectedly large radii for their masses, perhaps suggesting some presently unknown source of extra internal heating (Guillot & Showman 2002; Bodenheimer, Laughlin, & Lin 2003).”
• INFLATING HOT JUPITERS WITH OHMIC DISSIPATION (2010, background): “…tides (Bodenheimer et al. 2001), obliquity tides of a Cassini state (Winn & Holman 2005), and deposition of kinetic energy to adiabatic depths by dynamical and convective instabilities (Guillot & Showman 2002) have been invoked to provide an extra power source in the interior of the planet.”
• Evolutionary models for cool brown dwarfs and extrasolar giant planets. The case of HD 209458 (2003, background): “More recently, Guillot & Showman (2002) questioned such results and argue that the radius of HD209458b can only be reproduced if the deep atmosphere is much hotter than what can be expected from irradiation effects.”
• Possible Solutions to the Radius Anomalies of Transiting Giant Planets (2006, background): “Many workers have sought to explain the large radii of transiting planets such as HAT-P1b,WASP-1b, and HD 209458b by invoking an extra power source in the planet’s interior (Bodenheimer et al. 2003; Guillot & Showman 2002; Winn & Holman 2005; Chabrier et al. 2004; Charbonneau et al. 2007b).”