Strong tidal dissipation in Io and Jupiter from astrometric observations

Lainey, V.; Arlot, Jean-Eudes; Karatekin, Ö.; Hoolst, Tim Van

doi:10.1038/nature08108

Cited by 350 publications

(489 citation statements)

References 28 publications

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“…The elastic Love numbers were measured with accuracy only for the Earth and Mars, respectively, k e ≈ 0.3 (Mathews et al 1995), and k e ≈ 0.15 (Konopliv et al 2006). For the gaseous planets only the ratio k 2 /Q is known for Jupiter and Saturn, respectively, k 2 /Q ≈ 1.1 × 10 −5 (Lainey et al 2009), and k 2 /Q ≈ 2.3 × 10 −4 (Lainey et al 2012). The relaxation times are totally unknown for both terrestrial and gaseous planets, but if one is able to estimate Q, then τ and τ e can be estimated through expressions (46) and (56).…”

Section: Application To Close-in Planetsmentioning

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

110

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: Application To Close-in Planetsmentioning

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

110

186

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show abstract

“…In our final solution we use the theory of the motion of the Galilean satellites developed by Lainey et al (2009) Astrometric results of the observations may have the form of any corrected relative position of satellites X(t * ) = X th (t * ) + D x , Y(t * ) = Y th (t * ) + D y together with the associated time instant t * inside the time interval of the event. Although this is not mandatory, we assume that t * is the time instant when √ X 2 + Y 2 takes its minimum value, t * is the time of the closest apparent approach of the satellites.…”

Section: Extracting Astrometric Data From the Photometry Of Satellitementioning

confidence: 99%

The PHEMU09 catalogue and astrometric results of the observations of the mutual occultations and eclipses of the Galilean satellites of Jupiter made in 2009

Arlot¹,

Emelyanov²,

Varfolomeev³

et al. 2014

A&A

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Context. In 2009, the Sun and the Earth passed through the equatorial plane of Jupiter and therefore the orbital planes of its main satellites. It was the equinox on Jupiter. This occurrence made mutual occultations and eclipses between the satellites possible. Experience has shown that the observations of such events provide accurate astrometric data able to bring new information on the dynamics of the Galilean satellites. Observations are made under the form of photometric measurements, but need to be made through the organization of a worldwide observation campaign maximizing the number and the quality of the data obtained. Aims. This work focuses on processing the complete database of photometric observations of the mutual occultations and eclipses of the Galilean satellites of Jupiter made during the international campaign in 2009. The final goal is to derive new accurate astrometric data. Methods. We used an accurate photometric model of mutual events adequate with the accuracy of the observation. Our original method was applied to derive astrometric data from photometric observations of mutual occultations and eclipses of the Galilean satellites of Jupiter. Results. We processed the 457 lightcurves obtained during the international campaign of photometric observations of the Galilean satellites of Jupiter in 2009. Compared with the theory, for successful observations, the r.m.s. of O-C residuals are equal to 45.8 mas and 81.1 mas in right ascension and declination, respectively; the mean O-C residuals are equal to -2 mas and -9 mas in right ascension and declination, respectively, for mutual occultations; and -6 mas and +1 mas in right ascension and declination, respectively, for mutual eclipses.

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“…However, using the currently estimated tidal dissipation parameters to extrapolate backward in time predicts that the Moon was at Earth's surface about *2 Gyr ago (MacDonald, 1964), which contradicts the standard impact model for the lunar origin [note that numerous issues remain such as the origin of Earth's and the Moon's obliquities (Touma and Wisdom, 1994) and the perturbations from other planets (Ć uk, 2007)]. The deceleration of Io's orbital velocity has also been tentatively detected and seems broadly consistent with tidal theory (Aksnes and Franklin, 2001;Lainey et al, 2009). However, these data lie in the same regime, that of nearly circular orbits.…”

Section: Tidal Heatingmentioning

confidence: 85%

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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Strong tidal dissipation in Io and Jupiter from astrometric observations

Cited by 350 publications

References 28 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 PHEMU09 catalogue and astrometric results of the observations of the mutual occultations and eclipses of the Galilean satellites of Jupiter made in 2009

Tidal Venuses: Triggering a Climate Catastrophe via Tidal Heating

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