The Tethered Moon

  title={The Tethered Moon},
  author={K. Zahnle and R. Lupu and A. Dobrovolskis and N. Sleep},
  journal={Earth and Planetary Science Letters},
Abstract We address the thermal history of the Earth after the Moon-forming impact, taking tidal heating and thermal blanketing by the atmosphere into account. The atmosphere sets an upper bound of ∼100 W/m2 on how quickly the Earth can cool. The liquid magma ocean cools over 2–10 Myr, with longer times corresponding to high angular-momentum events. Tidal heating is focused mostly in mantle materials that are just beginning to freeze. The atmosphere's control over cooling sets up a negative… Expand
Thermal evolution of the early Moon
The early thermal evolution of Moon has been numerically simulated to understand the magnitude of the impact induced heating and the initially stored thermal energy of the accreting Moonlets. TheExpand
Tidal dissipation in the lunar magma ocean and its effect on the early evolution of the Earth–Moon system
Abstract The present-day inclination of the Moon reflects the entire history of its thermal and orbital evolution. The Moon likely possessed a global magma ocean following the Moon-forming impact. InExpand
A Model of the Primordial Lunar Atmosphere
Abstract We create the first quantitative model for the early lunar atmosphere, coupled with a magma ocean crystallization model. Immediately after formation, the moon's surface was subject to aExpand
Analytical Model for the Tidal Evolution of the Evection Resonance and the Timing of Resonance Escape
It is estimated that resonant escape occurs early, leading to only a small reduction in the Earth-Moon system angular momentum, as have been suggested previously. Expand
Giant impacts stochastically change the internal pressures of terrestrial planets
This work defines a new paradigm for pressure evolution during accretion of terrestrial planets: stochastic changes driven by impacts, using the Moon-forming impact as an example. Expand
Scaling in global tidal dissipation of the Earth-Moon system
Abstract The Moon migrated to cm over a characteristic time r / v = 10  Gyr by tidal interaction with Earth’s oceans at a present velocity of v = 3.8  cm yr − 1 . We model global dissipation to coverExpand
The energy budget and figure of Earth during recovery from the Moon-forming giant impact
Quantifying the energy budget of Earth in the first few million years following the Moon-forming giant impact is vital to understanding Earth's initial thermal state and the dynamics of lunar tidalExpand
On the origin of Earth's Moon
The Giant Impact is currently accepted as the leading theory for the formation of Earth's Moon. Successful scenarios for lunar origin should be able to explain the chemical composition of the MoonExpand
Near/Far Side Asymmetry in the Tidally Heated Moon.
A heat conductivity model illustrates that a moderately asymmetric and growing lunar crust could maintain its near/far side thickness asymmetry but only while the Moon is near the Earth. Expand
Collisionless encounters and the origin of the lunar inclination
It is shown that the modern lunar orbit provides a sensitive record of gravitational interactions with Earth-crossing planetesimals that were not yet accreted at the time of the Moon-forming event, and obviates the need for previously proposed excitation mechanisms and constrains the pristineness of the dynamical state of the Earth–Moon system. Expand


Emergence of a Habitable Planet
Abstract We address the first several hundred million years of Earth’s history. The Moon-forming impact left Earth enveloped in a hot silicate atmosphere that cooled and condensed over ∼1,000 yrs. AsExpand
Terrestrial aftermath of the Moon-forming impact
  • N. Sleep, K. Zahnle, R. Lupu
  • Geology, Medicine
  • Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences
  • 2014
The deep CO2 sequestration into the mantle could be explained by a rapid subduction of the old oceanic crust, such that the top of the crust would remain cold and retain its CO2. Expand
Magma ocean formation due to giant impacts
Current understanding of the last stages of planetary accretion suggests that mass and energy accumulation are dominated by a few large impacts. An important thermal consequence of such impacts isExpand
Evolution of a steam atmosphere during Earth's accretion.
The model assumes Safronov accretion, which includes degassing of planetesimals upon impact, thermal blanketing by a steam atmosphere, interchange of water between the surface and the interior, shock heating and convective cooling of Earth's interior, and hydrogen escape. Expand
It is now understood that the accretion of terrestrial planets naturally involves giant collisions, the moon-forming impact being a well-known example. In the aftermath of such collisions, theExpand
Thermal evolution of an early magma ocean in interaction with the atmosphere: conditions for the condensation of a water ocean
The thermal evolution of magma oceans produced by collision with giant impactors late in accretion is xpected to depend on the composition and structure of the atmosphere through the greenhouseExpand
Thermal and chemical evolution of the terrestrial magma ocean
Abstract The Earth is likely to have experienced a magma ocean stage during accretion. Thermal and chemical evolution of magma ocean is investigated based on a one-dimensional two-phase-flow heat andExpand
Equilibration in the aftermath of the lunar-forming giant impact
Abstract Simulations of the moon-forming impact suggest that most of the lunar material derives from the impactor rather than the Earth. Measurements of lunar samples, however, reveal an oxygenExpand
Initiation of clement surface conditions on the earliest Earth
How long this warm epoch lasted depends on how long a thick greenhouse atmosphere can be maintained by heat flow from the Earth's interior, either directly as a supplement to insolation, or indirectly through its influence on the nascent carbonate cycle. Expand
Impact-induced atmospheres and oceans on Earth and Venus
High-velocity impacts of planetesimals onto a growing planet result in the impact-degassing of volatiles and the formation of an impact-induced atmosphere. Because of the blanketing effect of such anExpand