Tidally Heated Terrestrial Exoplanets: Viscoelastic Response Models

Henning, W. G.; O’Connell, Richard J.; Sasselov, Dimitar

doi:10.1088/0004-637x/707/2/1000

Cited by 182 publications

(242 citation statements)

References 92 publications

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“…Storch & Lai 2014). For a review of the main viscoelastic models see Henning et al (2009). Efroimsky (2012) describes the rheology of a planet using an empirical power scaling law for the phase lag which is consistent with the accumulated geophysical, seismological, and geodetic observational data.…”

Section: Introductionmentioning

confidence: 84%

“…In this case, the planet can respond as an elastic solid or as a viscous fluid, depending on the frequency of the perturbation. Viscoelastic rheologies have been used recently (e.g., Henning et al 2009;Remus et al 2012a), since they are able to reproduce the main features of tidal dissipation, including the pseudo-synchronous rotation or the spin-orbit equilibria (e.g. Storch & Lai 2014).…”

Section: Introductionmentioning

confidence: 99%

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Deformation and tidal evolution of close-in planets and satellites using a Maxwell viscoelastic rheology

Correia

Boué

Laskar

et al. 2014

A&A

109

186

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In this paper we present a new approach to tidal theory. Assuming a Maxwell viscoelastic rheology, we compute the instantaneous deformation of celestial bodies using a differential equation for the gravity field coefficients. This method allows large eccentricities and it is not limited to quasi-periodic perturbations. It can take into account an extended class of perturbations, including chaotic motions and transient events. We apply our model to some already detected eccentric hot Jupiters and super-Earths in planar configurations. We show that when the relaxation time of the deformation is larger than the orbital period, spin-orbit equilibria arise naturally at half-integers of the mean motion, even for gaseous planets. In the case of super-Earths, these equilibria can be maintained for very low values of eccentricity. Our method can also be used to study planets with complex internal structures and other rheologies.

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Section: Introductionmentioning

confidence: 84%

Section: Introductionmentioning

confidence: 99%

Deformation and tidal evolution of close-in planets and satellites using a Maxwell viscoelastic rheology

Correia

Boué

Laskar

et al. 2014

A&A

109

186

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“…Even so, one may consider some boundary values defining intervals in which the viscoelastic parameters, of the used Maxwell rheological model, are likely to take their values. In RMZL12, we estimated such ranges based on our present knowledge of the rheology of the Earth mantle and the icy satellites of Jupiter (Henning et al 2009;Tobie 2003).…”

Section: Internal Structure Parametersmentioning

confidence: 99%

The surface signature of the tidal dissipation of the core in a two-layer planet

Remus

Mathis

Zahn

et al. 2014

A&A

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Context. Tidal dissipation, which is directly linked to internal structure, is one of the key physical mechanisms that drive the evolution of systems and govern their architecture. A robust evaluation of its amplitude is thus needed to predict the evolution time for spins and orbits and their final states. Aims. The purpose of this paper is to refine a recent model of the anelastic tidal dissipation in the central dense region of giant planets, which are commonly assumed to retain a large amount of heavy elements, which constitute an important source of dissipation. Methods. The previous paper evaluated the impact of the static fluid envelope on the tidal deformation of the core and on the associated anelastic tidal dissipation through the tidal quality factor Q c . We examine here its impact on the corresponding effective anelastic tidal dissipation through the effective tidal quality factor Q p . Results. We show that the strength of this mechanism mainly depends on mass concentration. In the case of Jupiter-and Saturnlike planets, it can increase their effective tidal dissipation by, around, factors 2.4 and 2, respectively. In particular, the range of the rheologies compatible with the observations is enlarged compared to the results issued from previous formulations. Conclusions. We derive here an improved expression of the tidal effective factor Q p in terms of the tidal dissipation factor of the core Q c , without assuming the commonly used assumptions. When applied to giant planets, the formulation obtained here allows a better match between the anelastic core's tidal dissipation of a two-layer model and the observations. Key words. planetary systems -planets and satellites: gaseous planets -planets and satellites: dynamical evolution and stabilityplanets and satellites: interiors -planets and satellites: general -planet-star interactions

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“…While simple and linear, such models are probably commensurate with the dearth of information we have about exoplanet interior processes. More complicated models have been constructed, and they reproduce the above models for certain choices of internal composition, structure, and energy transport (e.g., Henning et al, 2009). Thus, the CPL and CTL models can provide important and accurate insight into the tidal evolution of exoplanets.…”

Section: Tidal Heatingmentioning

confidence: 99%

“…Nonetheless, future work should explore these details. Henning et al (2009) performed detailed calculations and argued that k 2 = 0.3 and Q = 50 are reasonable choices for dry planets.…”

Section: E4 Tidal Response In Celestial Bodiesmentioning

confidence: 99%

Tidal Venuses: Triggering a Climate Catastrophe via Tidal Heating

et al. 2013

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Traditionally, stellar radiation has been the only heat source considered capable of determining global climate on long timescales. Here, we show that terrestrial exoplanets orbiting low-mass stars may be tidally heated at highenough levels to induce a runaway greenhouse for a long-enough duration for all the hydrogen to escape. Without hydrogen, the planet no longer has water and cannot support life. We call these planets ''Tidal Venuses'' and the phenomenon a ''tidal greenhouse.'' Tidal effects also circularize the orbit, which decreases tidal heating. Hence, some planets may form with large eccentricity, with its accompanying large tidal heating, and lose their water, but eventually settle into nearly circular orbits (i.e., with negligible tidal heating) in the habitable zone (HZ). However, these planets are not habitable, as past tidal heating desiccated them, and hence should not be ranked highly for detailed follow-up observations aimed at detecting biosignatures. We simulated the evolution of hypothetical planetary systems in a quasi-continuous parameter distribution and found that we could constrain the history of the system by statistical arguments. Planets orbiting stars with masses < 0.3 M Sun may be in danger of desiccation via tidal heating. We have applied these concepts to Gl 667C c, a *4.5 M Earth planet orbiting a 0.3 M Sun star at 0.12 AU. We found that it probably did not lose its water via tidal heating, as orbital stability is unlikely for the high eccentricities required for the tidal greenhouse. As the inner edge of the HZ is defined by the onset of a runaway or moist greenhouse powered by radiation, our results represent a fundamental revision to the HZ for noncircular orbits. In the appendices we review (a) the moist and runaway greenhouses, (b) hydrogen escape, (c) stellar mass-radius and mass-luminosity relations, (d) terrestrial planet mass-radius relations, and (e) linear tidal theories.

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Tidally Heated Terrestrial Exoplanets: Viscoelastic Response Models

Cited by 182 publications

References 92 publications

Deformation and tidal evolution of close-in planets and satellites using a Maxwell viscoelastic rheology

Deformation and tidal evolution of close-in planets and satellites using a Maxwell viscoelastic rheology

The surface signature of the tidal dissipation of the core in a two-layer planet

Tidal Venuses: Triggering a Climate Catastrophe via Tidal Heating

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