Solar System Dynamics

Murray, C. D.; Dermott, S. F.

doi:10.1017/cbo9781139174817

Cited by 2,307 publications

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“…Since our force is strictly radial, it does not affect the AM of the lunar orbit, in agreement with previous treatments of satellite tides 39 .…”

Section: Methodssupporting

confidence: 91%

“…This is the analytical expression for the eccentricity damping expected from radial tides for a moon in synchronous rotation 39 . While our radial force approximates the predicted damping of eccentricity to lowest order, our approach is fundamentally different from that taken in analytical derivation.…”

Section: Methodsmentioning

confidence: 99%

“…where f is the Moon's true anomaly, and the expression for the eccentricity damping by generalized accelerations 39,46 :…”

Section: Methodsmentioning

confidence: 99%

“…We may be tempted to apply this equation to the synchronous case, and assume that the lag-angle is independent of synodic frequency (equivalent to having constant Q) so that the angular acceleration simply changes sign when the rotation is slower than orbital motion 39 . We can estimate the effect of such tidal acceleration on eccentricity (with obliquity set to zero), using Eq.…”

Section: Methodsmentioning

confidence: 99%

“…As e E varies rapidly on 10 5 -yr timescales due to Milanković cycles 39 , capture is impossible and the Moon crosses the resonance many times in both directions. These numerous crossings result in a random walk in lunar eccentricity, within a band in a and e associated with the resonance 38 .…”

Section: Excitation Of Lunar Inclination By Encounters With Planetesimentioning

confidence: 99%

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Tidal evolution of the Moon from a high-obliquity, high-angular-momentum Earth

Ćuk

Hamilton

Lock

et al. 2016

Nature

124

103

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In the giant impact hypothesis for lunar origin, the Moon accreted from an equatorial circumterrestrial disk; however the current lunar orbital inclination of 5 • requires a subsequent dynamical process that is still debated [1][2][3] . In addition, the giant impact theory has been challenged by the Moon's unexpectedly Earth-like isotopic composition 4, 5 . Here, we show that tidal dissipation due to lunar obliquity was an important effect during the Moon's tidal evolution, and the past lunar inclination must have been very large, defying theoretical explanations. We present a new tidal evolution model starting with the Moon in an equatorial orbit around an initially fast-spinning, high-obliquity Earth, which is a probable outcome of giant impacts. Using numerical modeling, we show that the solar perturbations on the Moon's orbit naturally induce a large lunar inclination and remove angular momentum from the 1 arXiv:1802.03356v1 [astro-ph.EP] 9 Feb 2018Earth-Moon system. Our tidal evolution model supports recent high-angular momentum giant impact scenarios to explain the Moon's isotopic composition [6][7][8] and provides a new pathway to reach Earth's climatically favorable low obliquity.The leading theory for lunar origin is the giant impact 9, 10 , which explains the Moon's large relative size and small iron core. Here we refer to the giant impact theory in which the Earth-Moon post-impact angular momentum (AM) was the same as it is now (in agreement with classic lunar tidal evolution studies 11, 12 ) as "canonical". In the canonical giant impact model 13 , a Mars-mass body obliquely impacts the proto-Earth near the escape velocity to generate a circum-terrestrial debris disk. The angular momentum of the system is set by the impact, and the Moon accretes from the disk, which is predominantly (> 60 wt%) composed of impactor material. However, Earth and the Moon share nearly identical isotope ratios for a wide range of elements, and this isotopic signature is distinct from all other extraterrestrial materials 4, 5 . Because isotopic variations arise from multiple processes 4 , the Moon must have formed from, or equilibrated with, Earth's mantle 5,14 . Earth-Moon isotopic equilibration in the canonical model has been proposed by Pahlevan and Stevenson 15 , but has been questioned by other researchers 16 , who suggest that the large amount of mass exchange required to homogenize isotopes could lead to the collapse of the proto-lunar disk.Cuk and Stewart 6 proposed a new variant of the giant impact that is based on an initially high AM Earth-Moon system. In this model, a late erosive impact onto a fast-spinning proto-Earth produced a disk that was massive enough to form the Moon, and was composed primarily of material from Earth, potentially satisfying the isotopic observations. Canup 7 presented a variation of a high-2 AM origin in which a slow collision between two similar-mass bodies produces a fast-spinning Earth and disk with Earth-like composition. Subsequently, Lock et al. 8 have argued that a range of hig...

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“…Since our force is strictly radial, it does not affect the AM of the lunar orbit, in agreement with previous treatments of satellite tides 39 .…”

Section: Methodssupporting

confidence: 91%

Section: Methodsmentioning

confidence: 99%

“…where f is the Moon's true anomaly, and the expression for the eccentricity damping by generalized accelerations 39,46 :…”

Section: Methodsmentioning

confidence: 99%

Section: Methodsmentioning

confidence: 99%

Section: Excitation Of Lunar Inclination By Encounters With Planetesimentioning

confidence: 99%

See 3 more Smart Citations

Tidal evolution of the Moon from a high-obliquity, high-angular-momentum Earth

Ćuk

Hamilton

Lock

et al. 2016

Nature

124

103

View full text Add to dashboard Cite

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The tides of Mercury and possible implications for its interior structure

et al. 2014

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Key Points:• We present models of the tidal deformation of Mercury based on MESSENGER results • Tides are sensitive to size and density of the core and rheology of outer shell • The presence of a FeS layer would increase the tidal response AbstractThe combination of the radio tracking of the MErcury Surface, Space ENvironment, GEochemistry, and Ranging spacecraft and Earth-based radar measurements of the planet's spin state gives three fundamental quantities for the determination of the interior structure of Mercury: mean density , moment of inertia C, and moment of inertia of the outer solid shell C m . This work focuses on the additional information that can be gained by a determination of the change in gravitational potential due to planetary tides, as parameterized by the tidal potential Love number k 2 . We investigate the tidal response for sets of interior models that are compatible with the available constraints ( , C, and C m ). We show that the tidal response correlates with the size of the liquid core and the mean density of material below the outer solid shell and that it is affected by the rheology of the outer solid shell of the planet, which depends on its temperature and mineralogy. For a mantle grain size of 1 cm, we calculate that the tidal k 2 of Mercury is in the range 0.45 to 0.52. Some of the current models for the interior structure of Mercury are compatible with the existence of a solid FeS layer at the top of the core. Such a layer, if present, would increase the tidal response of the planet.

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Dynamics and distribution of Jovian dust ejected from the Galilean satellites

et al. 2016

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In this paper, the dynamical analysis of the Jovian dust originating from the four Galilean moons is presented. High‐accuracy orbital integrations of dust particles are used to determine their dynamical evolution. A variety of forces are taken into account, including the Lorentz force, solar radiation pressure, Poynting‐Robertson drag, solar gravity, the satellites' gravity, plasma drag, and gravitational effects due to nonsphericity of Jupiter. More than 20,000 dust particles from each source moon in the size range from 0.05 μm to 1 cm are simulated over 8000 (Earth) years until each dust grain hits a sink (moons, Jupiter, or escape from the system). Configurations of dust number density in the Jovicentric equatorial inertial frame are calculated and shown. In a Jovicentric frame rotating with the Sun the dust distributions are found to be asymmetric. For certain small particle sizes, the dust population is displaced towards the Sun, while for certain larger sizes, the dust population is displaced away from the Sun. The average lifetime as a function of particle size for ejecta from each source moon is derived, and two sharp jumps in the average lifetime are analyzed. Transport of dust between the Galilean moons and to Jupiter is investigated. Most of the orbits for dust particles from Galilean moons are prograde, while, surprisingly, a small fraction of orbits are found to become retrograde mainly due to solar radiation pressure and Lorentz force. The distribution of orbital elements is also analyzed.

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Solar System Dynamics

Cited by 2,307 publications

References 0 publications

Tidal evolution of the Moon from a high-obliquity, high-angular-momentum Earth

Tidal evolution of the Moon from a high-obliquity, high-angular-momentum Earth

The tides of Mercury and possible implications for its interior structure

Dynamics and distribution of Jovian dust ejected from the Galilean satellites

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