Classification of Satellite Resonances in the Solar System

Luan, Jing; Goldreich, Peter

doi:10.3847/1538-3881/153/1/17

Cited by 4 publications

(2 citation statements)

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“…However, it should migrate outward together with its MMR companion, Tethys. Luan & Goldreich (2017) Convergent migration is necessary for MMR capture. Assuming both satellites migrate due to resonance locking before they get caught in a MMR, the corresponding oscillations of Saturn must evolve convergently in the frequency domain.…”

Section: Mean Motion Resonancementioning

confidence: 99%

How Cassini can constrain tidal dissipation in Saturn

Luan

Fuller

Quataert

2017

Monthly Notices of the Royal Astronomical Society

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Tidal dissipation inside giant planets is important for the orbital evolution of their natural satellites. It is conventionally treated by parameterized equilibrium tidal theory, in which the tidal torque declines rapidly with distance, and orbital expansion was faster in the past. However, some Saturnian satellites are currently migrating outward faster than predicted by equilibrium tidal theory. Resonance locking between satellites and internal oscillations of Saturn naturally matches the observed migration rates. Here, we show that the resonance locking theory predicts dynamical tidal perturbations to Saturn's gravitational field in addition to those produced by equilibrium tidal bulges. We show that these perturbations can likely be detected during Cassini's proximal orbits if migration of satellites results from resonant gravity modes, but will likely be undetectable if migration results from inertial wave attractors or dissipation of the equilibrium tide. Additionally, we show that the detection of gravity modes would place constraints on the size of the hypothetical stably stratified region in Saturn.

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Section: Mean Motion Resonancementioning

confidence: 99%

How Cassini can constrain tidal dissipation in Saturn

Luan

Fuller

Quataert

2017

Monthly Notices of the Royal Astronomical Society

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“…Gallardo et al (2016) [10] have investigated three-body mean motion resonances for planetary and satellite by the semi-analytical method. Luan and Goldreich (2016) [17] have examined the classification of satellite resonances in the solar system for mean-motion resonances (MMRs). They have discussed the MMRs between Io-Europa, Europa-Ganymede, and Enceladus-Dione.…”

Section: Introductionmentioning

confidence: 99%

Dynamics of Resonant Curves of Earth-Moon system under the influence of Resistive Force using Unperturbed Solution

Yadav

Kumar

Aggarwal

et al. 2023

Preprint

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This work investigates the dynamical behavior of the resonant curves in the motion of the Earth-Moon system under the influence of resistive force. In this study, the resonance arises in this motion due to the rate of change of Earth’s equatorial ellipticity (EEE) (˙ γ), the Moon’s angular velocity (˙ θmo) around the Earth, and angular velocity of barycenter (˙ α0) around the Sun, including the coefficient of resistive force (b). The configuration and equations of motion are expressed in a spherical coordinate system using the Earth’s potential. Applying the unperturbed solution reduces and simplifies the system into a second-order ODE and obtains a particular solution. It is observe that the commensurability occur between the frequencies: (i) ˙ γ and ˙ θm0, (ii) ˙ θm0 and ˙ α0 with the coefficient of resistive force. Finally, we analyze the dynamical behavior of the resonant curves for the orbital elements and the coefficient of resistive force.

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