Tidal Evolution of the Evection Resonance/Quasi‐Resonance and the Angular Momentum of the Earth‐Moon System

Rufu, Raluca; Canup, R. M.

doi:10.1029/2019je006312

Cited by 23 publications

(8 citation statements)

References 47 publications

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“…Touma & Wisdom (1998) studied this regime and showed that capture into such a resonance could have been encountered for a M ≈ 4.6R E , exciting the lunar eccentricity to e ≈ 0.5. However, the timescale of capture and escape from this evection resonance is 10 4 ∼ 10 5 yr, after which the lunar orbit tends to circularization again (Rufu & Canup 2020).…”

Section: Appendix A: Orbital Dynamicsmentioning

confidence: 99%

The resonant tidal evolution of the Earth-Moon distance

Farhat

Auclair-Desrotour

Boué

et al. 2022

A&A

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Due to tidal interactions in the Earth-Moon system, the spin of the Earth slows down and the Moon drifts away. This recession of the Moon can now be measured with great precision, but it was noticed more than fifty years ago that simple tidal models extrapolated back in time lead to an age of the Moon that is largely incompatible with the geochronological and geochemical evidence. In order to evade this problem, more elaborate models have been proposed, taking into account the oceanic tidal dissipation. However, these models have not been able to fit both the estimated lunar age and the present rate of lunar recession simultaneously. In the present work, we present a physical model that reconciles these two constraints and yields a unique solution for the tidal history. This solution fits the available geological proxies for the history of the Earth-Moon system well and it consolidates the cyclostratigraphic method. Our work extends the lineage of earlier works on the analytical treatment of fluid tides on varying bounded surfaces that is further coupled with solid tidal deformations. This allows us to take into account the time-varying continental configuration on Earth by considering hemispherical and global ocean models. The resulting evolution of the Earth-Moon system involves multiple crossings of resonances in the oceanic dissipation that are associated with significant and rapid variations in the lunar orbital distance, the length of an Earth day and the Earth’s obliquity.

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Section: Appendix A: Orbital Dynamicsmentioning

confidence: 99%

The resonant tidal evolution of the Earth-Moon distance

Farhat

Auclair-Desrotour

Boué

et al. 2022

A&A

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show abstract

“…For non-spinning planets, the range of satellite-producing impact angles is only a few degrees, but for spinning planets, wider ranges become feasible. In particular, a prograde spinning proto-Earth allows less disruption of Theia for viable satellite formation at lower angles, although high initial rotation rates may require some angular momentum to be removed from the final system (Rufu & Canup 2020).…”

Section: Immediate Satellite Formationmentioning

confidence: 99%

“…High angular momentum impacts into rapidly spinning targets ( Ćuk & Stewart 2012;Lock et al 2018) can eject and mix more proto-Earth material, as can a very large impactor (Canup 2012). The excess angular momentum might be removable in or near the evection resonance, but removing the correct amount may be difficult (Rufu & Canup 2020). Hit-and-run impacts can also make somewhat more target-rich disks (Reufer et al 2012).…”

Section: Introductionmentioning

confidence: 99%

Immediate Origin of the Moon as a Post-impact Satellite

Kegerreis¹,

Ruiz-Bonilla²,

Eke³

et al. 2022

ApJL

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The Moon is traditionally thought to have coalesced from the debris ejected by a giant impact onto the early Earth. However, such models struggle to explain the similar isotopic compositions of Earth and lunar rocks at the same time as the system’s angular momentum, and the details of potential impact scenarios are hotly debated. Above a high resolution threshold for simulations, we find that giant impacts can immediately place a satellite with similar mass and iron content to the Moon into orbit far outside Earth’s Roche limit. Even satellites that initially pass within the Roche limit can reliably and predictably survive, by being partially stripped and then torqued onto wider, stable orbits. Furthermore, the outer layers of these directly formed satellites are molten over cooler interiors and are composed of around 60% proto-Earth material. This could alleviate the tension between the Moon’s Earth-like isotopic composition and the different signature expected for the impactor. Immediate formation opens up new options for the Moon’s early orbit and evolution, including the possibility of a highly tilted orbit to explain the lunar inclination, and offers a simpler, single-stage scenario for the origin of the Moon.

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“…While the total angular momentum of the bound material, a key constraint in case of the Moon forming GI (e.g., Canup 2004a), shows little variation for the two compared EOS and different resolutions, the Earth's post-impact rotation period affects the tidal interaction with the Moon. This in turn affects the Moon's outward migration rate and the efficiency of AM removal due to evection resonances (Rufu & Canup 2020), a key mechanism in reconciling high AM Moon forming impacts with observations (Canup 2012;Ćuk & Stewart 2012;Lock et al 2018). The impact conditions that lead to erosion of a proto-planet or smaller body are characterised by the value of 𝑄 * RD and play a crucial role in determining many important properties of the final planetary system like the final number of planets, their mass and bulk composition.…”

Section: Discussionmentioning

confidence: 99%

The EOS/Resolution Conspiracy: Convergence in Proto-Planetary Collision Simulations

Meier,

Reinhardt,

Stadel

2021

Preprint

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We investigate how the choice of equation of state (EOS) and resolution conspire to affect the outcomes of giant impact (GI) simulations. We focus on the simple case of equal mass collisions of two Earth-like 0.5 M ⊕ proto-planets showing that the choice of EOS has a profound impact on the outcome of such collisions as well as on the numerical convergence with resolution. In simulations where the Tillotson EOS is used, impacts generate an excess amount of vapour due to the lack of a thermodynamically consistent treatment of phase transitions and mixtures. In oblique collisions this enhances the artificial angular momentum (AM) transport from the planet to the circum-planetary disc reducing the planet's rotation period over time. Even at a resolution of 1.3 × 10 6 particles the result is not converged. In head-on collisions the lack of a proper treatment of the solid/liquid-vapour phase transition allows the bound material to expand to very low densities which in turn results in very slow numerical convergence of the critical specific impact energy for catastrophic disruption 𝑄 * RD with increasing resolution as reported in prior work. The simulations where ANEOS is used for oblique impacts are already converged at a modest resolution of 10 5 particles, while head-on collisions converge when they evidence the post-shock formation of a dense iron-rich ring, which promotes gravitational re-accumulation of material. Once sufficient resolution is reached to resolve the liquid-vapour phase transition of iron in the ANEOS case, and this ring is resolved, the value of 𝑄 * RD has then converged.

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Tidal Evolution of the Evection Resonance/Quasi‐Resonance and the Angular Momentum of the Earth‐Moon System

Cited by 23 publications

References 47 publications

The resonant tidal evolution of the Earth-Moon distance

The resonant tidal evolution of the Earth-Moon distance

Immediate Origin of the Moon as a Post-impact Satellite

The EOS/Resolution Conspiracy: Convergence in Proto-Planetary Collision Simulations

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