Spin evolution of Earth-sized exoplanets, including atmospheric tides and core–mantle friction

Cunha, Diana; Correia, A. C. M.; Laskar, Jacques

doi:10.1017/s1473550414000226

Cited by 47 publications

(31 citation statements)

References 118 publications

(135 reference statements)

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“…(136) 9 Aside from that, in the general case it is necessary to take into account the tidally-generated change in the orientation of the equator. As we shall see below, this will yield an additional term in the expression for di/dt , see equation (162).…”

Section: Expansion Of the Additional Tidal Potentialmentioning

confidence: 99%

“…Tolerable for the Earth-Moon system (which Kaula was having in mind), this approximation is unacceptable for a binary comprising partners of comparable masses. So, Kaula's expressions for the rates must be multiplied by (M + M ′ )/M , to compensate for that oversight 9. This redundant factor of M/(M + M ′ ) has become a source of inaccuracy in many publications.…”

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confidence: 99%

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Tidal evolution of the Keplerian elements

Boué

Efroimsky

2019

Celest Mech Dyn Astr

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We address the expressions for the rates of the Keplerian orbital elements within a two-body problem perturbed by the tides in both partners. Formulae for these rates have appeared in the literature in various forms, at times with errors. We reconsider, from scratch, the derivation of these rates and arrive at the Lagrange-type equations which, in some details, differ from the corresponding equations obtained previously by Kaula (1964).We also write down detailed expressions for da/dt , de/dt and di/dt , to order e 4 . They differ from Kaula's expressions which contain a redundant factor of M/(M + M ′ ) , with M and M ′ being the masses of the primary and the secondary. As Kaula was interested in the Earth-Moon system, this redundant factor was close to unity and was unimportant in his developments. This factor, however, must be removed when Kaula's theory is applied to a binary composed of partners of comparable masses.We have found that, while it is legitimate to simply sum the primary's and secondary's inputs in da/dt or de/dt , this is not the case for di/dt . So our expression for di/dt differs from that of Kaula in two regards. First, the contribution due to the dissipation in the secondary averages out when the apsidal precession is uniform. Second, we have obtained an additional term which emerges owing to the conservation of the angular momentum: a change in the inclination of the orbit causes a change of the primary's plane of equator.Recall that these expressions are general. In our case, the two-body problem perturbed by tides, H is independent of Θ and Θ ′ . So the partial derivatives of the Hamiltonian over these two quantities in equations (35) and (36) become zero. 9

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Section: Expansion Of the Additional Tidal Potentialmentioning

confidence: 99%

mentioning

confidence: 99%

Tidal evolution of the Keplerian elements

Boué

Efroimsky

2019

Celest Mech Dyn Astr

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“…Planets around M dwarfs are of particular interest because the dimness of the host stars means that their habitable zones (e.g., Kopparapu et al 2013) are located at short orbital periods, which are much more accessible to observational study . However, planets within the habitable zone of M dwarfs face additional challenges such as tidal locking and large incident fluxes of high-energy photons (Lammer et al 2003;Cunha et al 2015;Shields et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Detection of the Atmosphere of the 1.6 M_⊕ Exoplanet GJ 1132 b

Southworth

Mancini

Madhusudhan

et al. 2017

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Detecting the atmospheres of low-mass, low-temperature exoplanets is a high-priority goal on the path to ultimately detecting biosignatures in the atmospheres of habitable exoplanets. High-precision HST observations of several super-Earths with equilibrium temperatures below 1000 K have to date all resulted in featureless transmission spectra, which have been suggested to be due to high-altitude clouds. We report the detection of an atmospheric feature in the atmosphere of a 1.6 M Å transiting exoplanet, GJ 1132 b, with an equilibrium temperature of ∼600 K and orbiting a nearby M dwarf. We present observations of nine transits of the planet obtained simultaneously in the griz and JHK passbands. We find an average radius of 1.43±0.16 R Å for the planet, averaged over all the passbands, and a radius of 0.255±0.023 R  for the star, both of which are significantly greater than previously found. The planet radius can be decomposed into a "surface radius" at ∼1.375 R Å overlaid by atmospheric features that increase the observed radius in the z and K bands. The z-band radius is 4σ higher than the continuum, suggesting a strong detection of an atmosphere. We deploy a suite of tests to verify the reliability of the transmission spectrum, which are greatly helped by the existence of repeat observations. The large z-band transit depth indicates strong opacity from H 2 O and/or CH 4 or a hitherto-unconsidered opacity. A surface radius of 1.375±0.16 R Å allows for a wide range of interior compositions ranging from a nearly Earth-like rocky interior, with ∼70% silicate and ∼30% Fe, to a substantially H 2 O-rich water world.

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“…This same effect was also invoked to explain the retrograde spin of Venus (see Correia & Laskar 2001. However, for close-in planets, the gravitational tides dominate the thermal tides, so synchronous rotation is believed to be the most likely scenario (Correia et al 2008;Cunha et al 2015).…”

Section: Introductionmentioning

confidence: 81%

Spin dynamics of close-in planets exhibiting large transit timing variations

Delisle

Correia

Leleu

et al. 2017

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We study the spin evolution of close-in planets in compact multi-planetary systems. The rotation period of these planets is often assumed to be synchronous with the orbital period due to tidal dissipation. Here we show that planet-planet perturbations can drive the spin of these planets into non-synchronous or even chaotic states. In particular, we show that the transit timing variation (TTV) is a very good probe to study the spin dynamics, since both are dominated by the perturbations of the mean longitude of the planet. We apply our model to KOI-227 b and Kepler-88 b, which are both observed undergoing strong TTVs. We also perform numerical simulations of the spin evolution of these two planets. We show that for KOI-227 b non-synchronous rotation is possible, while for Kepler-88 b the rotation can be chaotic.

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Spin evolution of Earth-sized exoplanets, including atmospheric tides and core–mantle friction

Cited by 47 publications

References 118 publications

Tidal evolution of the Keplerian elements

Tidal evolution of the Keplerian elements

Detection of the Atmosphere of the 1.6 M_⊕ Exoplanet GJ 1132 b

Spin dynamics of close-in planets exhibiting large transit timing variations

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Spin evolution of Earth-sized exoplanets, including atmospheric tides and core–mantle friction

Cited by 47 publications

References 118 publications

Tidal evolution of the Keplerian elements

Tidal evolution of the Keplerian elements

Detection of the Atmosphere of the 1.6 M⊕ Exoplanet GJ 1132 b

Spin dynamics of close-in planets exhibiting large transit timing variations

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Product

Resources

About

Detection of the Atmosphere of the 1.6 M_⊕ Exoplanet GJ 1132 b