Tides on Satellites of Giant Planets

Rambaux, N.; Castillo‐Rogez, Julie

doi:10.1007/978-3-642-32961-6_5

Cited by 10 publications

(14 citation statements)

References 118 publications

(197 reference statements)

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“…The Moon is an example of tidal dissipation in a silicate body. The larger population of solar system planets and satellites [ Rambaux and Castillo‐Rogez , ; Mathis et al ., ] as well as exoplanets [ Henning et al ., ] has a variety of compositions, structures, temperatures, pressures, time scales, and tidal strengths. The Earth is another silicate body, and similarities between the terrestrial D′′ layer at the base of the mantle and the lunar attenuation zone are intriguing.…”

Section: Future Investigationsmentioning

confidence: 99%

Tides on the Moon: Theory and determination of dissipation

2015

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Solid body tides on the Moon vary by about ±0.1 m each month. In addition to changes in shape, the Moon's gravity field and orientation in space are affected by tides. The tidal expressions for an elastic sphere are compact, but dissipation introduces modifications that depend on the forcing period. Consequently, a Fourier representation of the tide-raising potential is needed. A mathematical model for the distortion-caused tidal potential may be used for the analysis of precise spacecraft tracking data. Since tides affect gravitational torques on the Moon from the Earth's attraction, the lunar orientation is also affected. Expressions for five periodic perturbations of orientation are presented. The rheological properties of lunar materials determine how the Moon responds to different tidal periods. New lunar laser ranging solutions for the tidal orientation terms are presented. The quality factor Q is 38 ± 4 at 1 month, 41 ± 9 at 1 year, ≥74 at 3 years, and ≥58 at 6 years. The ranging results can be matched with absorption band models that peak at 120 days and single relaxation time models that peak at~100 days. Combined models are possibilities. Dissipation can modify laser ranging solutions; previously reported core flattening is too uncertain to be useful. Strong lunar tidal dissipation, modeled to arise in the deep hot mantle, appears to be from a region with radius ≥535 km. Classical Maxwell-type dissipation is too weak to detect at 3 and 6 year periods.

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Section: Future Investigationsmentioning

confidence: 99%

Tides on the Moon: Theory and determination of dissipation

2015

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“…Currently, Ganymede's deformation expressed through the Love numbers k 2 and h 2 and their phase lags are not known (e.g., Rambaux and Castillo-Rogez 2013). Measurements of the Love numbers by the JUICE mission (Grasset et al 2013) will constrain the thickness and elastic behavior of the ice shell and the phase lags will reveal the presence of a global ocean and could inform on the thermal state of the deeper interior (Kamata et al 2016;Hussmann et al 2016).…”

Section: Ganymedementioning

confidence: 99%

Interiors of Earth-Like Planets and Satellites of the Solar System

Breuer¹,

Spohn

Hoolst

et al. 2021

Surv Geophys

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The Earth-like planets and moons in our solar system have iron-rich cores, silicate mantles, and a basaltic crust. Differentiated icy moons can have a core and a mantle and an outer water–ice layer. Indirect evidence for several icy moons suggests that this ice is underlain by or includes a water-rich ocean. Similar processes are at work in the interiors of these planets and moons, including heat transport by conduction and convection, melting and volcanism, and magnetic field generation. There are significant differences in detail, though, in both bulk chemical compositions and relative volume of metal, rock and ice reservoirs. For example, the Moon has a small core [~ 0.2 planetary radii (RP)], whereas Mercury’s is large (~ 0.8 RP). Planetary heat engines can operate in somewhat different ways affecting the evolution of the planetary bodies. Mercury and Ganymede have a present-day magnetic field while the core dynamo ceased to operate billions of years ago in the Moon and Mars. Planets and moons differ in tectonic style, from plate-tectonics on Earth to bodies having a stagnant outer lid and possibly solid-state convection underneath, with implications for their magmatic and atmosphere evolution. Knowledge about their deep interiors has improved considerably thanks to a multitude of planetary space missions but, in comparison with Earth, the data base is still limited. We describe methods (including experimental approaches and numerical modeling) and data (e.g., gravity field, rotational state, seismic signals, magnetic field, heat flux, and chemical compositions) used from missions and ground-based observations to explore the deep interiors, their dynamics and evolution and describe as examples Mercury, Venus, Moon, Mars, Ganymede and Enceladus.

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“…In planetary systems with many satellites such as as the Jovian and Saturnian systems, a body not only interacts with its parent planet but also with all the other moons. Some of them are in what is called a Laplace resonance, which is a stable situation where the orbit rates of several moons are multiples of one another (Rambaux & Castillo-Rogez, 2013).…”

Section: Libration Of Moonsmentioning

confidence: 99%

Rotational Dynamics of Planetary Cores: Instabilities Driven By Precession, Libration and Tides

Reun

Bars

2019

Fluid Mechanics of Planets and Stars

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In this chapter, we explore how gravitational interactions drive turbulent flows inside planetary cores and provide an interesting alternative to convection to explain dynamo action and magnetic fields around terrestrial bodies. In the first section, we introduce tidal interactions and their effects on the shape and rotation of astrophysical bodies. A method is given to derive the primary response of liquid interiors to these tidally-driven perturbations. In the second section, we detail the stability of this primary response and demonstrate that it is able to drive resonance of inertial waves. As the instability mechanism is introduced, we draw an analogy with the parametric amplification of a pendulum whose length is periodically varied. Lastly, we present recent results regarding this instability, in particular its non-linear saturation and its ability to drive dynamo action. We present how it has proved helpful to explain the magnetic field of the early Moon.

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Tides on Satellites of Giant Planets

Cited by 10 publications

References 118 publications

Tides on the Moon: Theory and determination of dissipation

Tides on the Moon: Theory and determination of dissipation

Interiors of Earth-Like Planets and Satellites of the Solar System

Rotational Dynamics of Planetary Cores: Instabilities Driven By Precession, Libration and Tides

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