On the Tidal Inflation of Short-Period Extrasolar Planets

By P. Bodenheimer, D. Lin, Rosemary A. Mardling. 2001

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In Astronomy and Astrophysics

Citations in the corpus

TIDAL EVOLUTION OF CLOSE-IN PLANETS (2010, background): “The orbits of these planets might have been circularized as the planet lost mass (e.g. Lammer et al. 2003; Lecavelier Des Etangs 2007), or the planetary radius expanded due to tidal heating (e.g. Bodenheimer et al. 2001; Gu et al. 2003).”
Two Classes of Hot Jupiters (2007, background): “This is the well-known anomaly that was first identified with the detection of the first transiting planet, HD209458b (Bodenheimer et al. 2001;Guillot&Showman2002).”
The 3.6-8.0 μm Broadband Emission Spectrum of HD 209458b: Evidence for an Atmospheric Temperature Inversion (2007, background): “Given that there is a clear distinction between hot Jupiters with inflated radii and those with normal (i.e. consistent with models) radii, a comparative study of the infrared emission spectra of the planets in these two classes might reveal important differences.”
Is tidal heating sufficient to explain bloated exoplanets? Consistent calculations accounting for finite initial eccentricity (2010, background): “As a result, tides raised in an eccentric planet can slow down its contraction (Bodenheimer et al. 2001; Leconte et al. 2009; Baraffe et al. 2010) or even lead to a transitory phase of expansion (Miller et al. 2009; Ibgui et al. 2009).”
Calculating the Tidal, Spin, and Dynamical Evolution of Extrasolar Planetary Systems (2002, methodology): “The luminosity of the planet L is therefore given by the inverse of equation (1) in Bodenheimer et al. (2001) [in fact, we refit the data for the inverse and calculate a fifth-order polynomial for log ðL=L Þ vs. log ðS2=R Þ].”
THE MASS OF KOI-94d AND A RELATION FOR PLANET RADIUS, MASS, AND INCIDENT FLUX (2013, unknown): “Coupled tidal and planetary structure evolution has been calculated by a number of authors (Bodenheimer et al. 2001; Gu et al. 2003; Ibgui & Burrows 2009; Miller et al. 2009; Ibgui et al. 2010; Leconte et al. 2010).”
The Transit Light Curve Project. I. Four Consecutive Transits of the Exoplanet XO-1b (2006, background): “Other explanations, such as ongoing tidal circularization due to an eccentricity exchange with a third body (Bodenheimer et al. 2001), or the trapping in a Cassini state with nonzero obliquity (Winn & Holman 2005), would seemingly have difficulty accounting for a large population of inflated…”
On the tidal evolution of Hot Jupiters on inclined orbits (2009, background): “It has been proposed that H2 can result in planetary inflation, c© 2009 RAS, MNRAS 000, 1–?? if the energy is deposited deep in the interior of the planet (Bodenheimer et al. 2001; Jackson et al. 2008b).”
Tidal Dissipation in Stars and Giant Planets (2014, background): “…of Jupiter’s moon Io and Saturn’s moon Enceladus, this effect has been investigated mainly for short-period extrasolar planets undergoing tidal circularization, in an attempt to explain the unexpectedly large radii of many transiting planets (e.g. Bodenheimer et al. 2001; Ibgui & Burrows 2009).”
On the Radii of Extrasolar Giant Planets (2003, methodology): “The required dissipation is higher than that quoted by Bodenheimer et al. (2001) because of changes in the equation of state and opacity since that time.”
INFLATING HOT JUPITERS WITH OHMIC DISSIPATION (2010, background): “…gas giants require between 10−6 and 10−2 of the irradiation they receive to be deposited into the adiabatic interior to maintain their radii (Bodenheimer et al. 2001; Burrows et al. 2007; Ibgui et al. 2009), although the exact number depends on the metallicity of the atmosphere and the…”
Atmospheric circulation and tides of ``51 Pegasus b-like'' planets (2002, background): “In that case, the energy dissipated becomes Ė ∼ 1024 erg sec−1, which is two orders of magnitude smaller than that necessary to significantly affect the planet’s evolution (Paper I; Bodenheimer et al. 2001).”
OBSERVATIONAL EVIDENCE FOR TIDAL DESTRUCTION OF EXOPLANETS (2009, background): “…example, tidal heating may be sufficient to account for many of the discrepancies between the predicted and observed radii of transiting exoplanets (Bodenheimer et al. 2001; Bodenheimer et al. 2003; Burrows et al. 2007; Jackson et al. 2008b; Liu et al. 2008; Ibgui & Burrows 2009; Miller et al.…”
Spin-Orbit Evolution of Short-Period Planets (2004, background): “The dissipation of these disturbances leads not only to dynamical changes but also to internal heating, which may cause them to inflate (Bodenheimer et al. 2001).”
Observational Evidence for Tidal Interaction in Close Binary Systems (2007, background): “The conjecture was that a small eccentricity of HD 209458b orbit (e.g., Laughlin et al. 2005) causes tidal dissipation inside the planet, which serves as another source of energy that inflates the planet (e.g., Bodenheimer et al. 2001; Bedenheimer et al. 2003; Gu et al. 2004; Mardling 2007).”
The Interior Structure, Composition, and Evolution of Giant Planets (2009, background): “– Bodenheimer et al. (2001) proposed that the radius of HD 209458b could be ex- plained by non-zero orbital eccentricity, forced by an unseen additional planetary companion.”