Tidal heating in Enceladus

Meyer, Jennifer; Wisdom, Jack

doi:10.1016/j.icarus.2007.03.001

Cited by 159 publications

(162 citation statements)

References 13 publications

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“…We have shown that equilibrium tidal heating in Enceladus cannot account for the nonsolar heat emanating from Enceladus (Meyer and Wisdom, 2007): equilibrium tidal heating can account for only 1.1(18000/Q S ) GW of the observed 5.8±1.9 GW (Spencer et al, 2006). Provided the origin of the observed heating is tidal heating, it is possible that Enceladus is oscillating about equilibrium.…”

Section: Introductionmentioning

confidence: 83%

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Episodic volcanism on Enceladus: Application of the Ojakangas–Stevenson model

Meyer¹,

Wisdom²

2008

Icarus

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Section: Introductionmentioning

confidence: 83%

“…where m = (L + 4)/3, and β = 13 for Io in the Io-EuropaGanymede resonance and β = 30.69 for Enceladus in the Enceladus-Dione resonance (Meyer and Wisdom, 2007). The equilibrium value of the square of the eccentricity is…”

Section: Ojakangas and Stevenson Evolution Equationsmentioning

confidence: 99%

Episodic volcanism on Enceladus: Application of the Ojakangas–Stevenson model

Meyer¹,

Wisdom²

2008

Icarus

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“…The intensity of the geysers of Enceladus depends on how close or far the satellite is from Saturn [47].…”

Section: Discussion Of Some Detail Related To the Estimation Of The Rmentioning

confidence: 99%

Superconductivity of Saturn Rings: Quantum Locking, Rings Disc Thickness and Its Time Creation

Tchernyi¹,

Pospelov²

2018

JMP

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The article demonstrates how rings disc of Saturn was created after appearance of the planetary magnetic field from superconducting iced particles of the protoplanetary cloud moving around planet by chaotic orbits. It is based on the fact that Saturn has magnetic field and the temperature of its vicinity is low enough to have superconductivity. Electromagnetic simulation estimates time of rings disc formation with the thickness about few meters from a few thousand years up to few tens of thousands of years. A rings disk has a stable structure located within magnetic equator of Saturn due to quantum locking of the particles by planetary magnetic field. Also may happened contribution to the rings disc from the debris of the moons migrated inward towards Saturn and particles of the frozen water coming from the geyser of the geologically active satellite (as Enceladus contributed to the E-ring). Suggested mechanism of the rings formation works even in case where only a small fraction of the particles poses superconductivity. Presented electromagnetic modeling of the role of superconducting iced particles of the rings disc origin, dynamics and evolution allow us to enrich the classical theories based on gravitational, mechanical, magnetohydrodynamic and plasma interactions.

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“…The Cassini probe has observed that Enceladus is a currently active body emanating water plumes, possibly implying liquid water in its subsurface (e.g., Porco et al 2006). If Enceladus is in an equilibrium state of the resonance with Dione, the tidal heating rate generated in Enceladus is ∼1.1 GW at Q s = 18 000 (Meyer & Wisdom 2007), which is independent of the interior structure of Enceladus. However, the equilibrium heating rate increases with decreasing Q s (Meyer & Wisdom 2007;Lainey et al 2012), which may affect Enceladus' structure and activity.…”

Section: Introductionmentioning

confidence: 95%

Frequency-dependent tidal dissipation in a viscoelastic Saturnian core and expansion of Mimas’ semi-major axis

Dake¹,

Hußmann²

2017

A&A

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Context. Regarding tidal dissipation in Saturn, usually parameterized by Saturn's quality factor Q, there remains a discrepancy between conventional estimates and the latest determination that has been derived from astrometric observations of Saturn's inner satellites. If dissipation in Saturn is as large as the astrometric observations suggest, and is independent of time and tidal frequency, conventional models predict that Mimas' initial orbit should be located inside Saturn's synchronous orbit or even inside its Roche limit, in contradiction to formation models. Aims. Using simple structure models and assuming Saturn's core to be viscoelastic, we look for dissipation models which are consistent with both the latest astrometric observations and with Mimas' orbital migration. Methods. Firstly, using a two-layer model of Saturn's interior structure, we constrain the ranges of rigidity and viscosity of Saturn's core which are consistent with Saturn's dissipation derived from astrometric observations at the tidal frequencies of Enceladus, Tethys, and Dione. Next, within the constrained viscosity and rigidity ranges, we calculate Mimas' semi-major axis considering the frequency dependence of viscoelastic dissipation in Saturn's core. By the two calculations, we evaluate (1) Saturnian models which can explain the astrometrically determined Saturnian dissipation, and (2) whether Mimas' initial semi-major axis is larger than the synchronous orbit. Results. We show that if the core is assumed to be solid with a viscosity of 10 13 −10 14 Pa s (depending on its size), the lower boundary of the observed Saturnian dissipation at tidal frequencies of Enceladus, Tethys, and Dione (k 2s /Q s ∼ 4 × 10 −5 where k 2s is Saturn's second degree Love number and Q s its quality factor) can be explained by our model. In this viscosity range, Mimas can stay outside the synchronous orbit and the Roche limit for 4.5 billion years of evolution. Conclusions. In the case of a frequency dependent viscoelastic dissipative core, the lower boundary of the observed Saturnian dissipation can be consistent with the orbital expansion of Mimas. In this model, the assumption of a late formation of Mimas, discussed recently, is not required.

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Tidal heating in Enceladus

Cited by 159 publications

References 13 publications

Episodic volcanism on Enceladus: Application of the Ojakangas–Stevenson model

Episodic volcanism on Enceladus: Application of the Ojakangas–Stevenson model

Superconductivity of Saturn Rings: Quantum Locking, Rings Disc Thickness and Its Time Creation

Frequency-dependent tidal dissipation in a viscoelastic Saturnian core and expansion of Mimas’ semi-major axis

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