none 10.1029/2021JE006875 American Geophysical Union (AGU) American Geophysical Union 13 130442443 212447 2023082306072900213 10.1029 2023-08-24T03:13:50Z 2021-09-23T23:10:15Z 53 Journal of Geophysical Research: Planets JGR Planets 2169-9097 2169-9100 12 2021 126 12 Houraa Daher Department of Climate and Space Sciences and Engineering University of Michigan Ann Arbor MI USA Rosenstiel School for Marine and Atmospheric Science University of Miami Miami FL USA https://orcid.org/0000-0002-0017-7346 Brian K. Arbic Department of Earth and Environmental Sciences University of Michigan Ann Arbor MI USA Institut des Géosciences de L'Environnement (IGE) Grenoble France Laboratoire des Etudes en Géophysique et Océanographie Spatiale (LEGOS) Toulouse France https://orcid.org/0000-0002-7969-2294 James G. Williams Jet Propulsion Laboratory California Institute of Technology Pasadena CA USA https://orcid.org/0000-0002-8441-5937 Joseph K. Ansong Department of Earth and Environmental Sciences University of Michigan Ann Arbor MI USA Department of Mathematics University of Ghana Accra Ghana https://orcid.org/0000-0002-2214-377X Dale H. Boggs Jet Propulsion Laboratory California Institute of Technology Pasadena CA USA https://orcid.org/0000-0002-1568-3428 Malte Müller Norwegian Meteorological Institute Oslo Norway https://orcid.org/0000-0003-2871-8359 Michael Schindelegger Institute of Geodesy and Geoinformation University of Bonn Bonn Germany https://orcid.org/0000-0001-6250-7921 Jacqueline Austermann Department of Earth and Environmental Sciences Columbia University New York NY USA https://orcid.org/0000-0003-3754-5082 Bruce D. Cornuelle Scripps Institution of Oceanography University of California La Jolla CA USA Eliana B. Crawford Department of Earth and Environmental Sciences University of Michigan Ann Arbor MI USA Swift Navigation San Francisco CA USA Department of Physics Kenyon College Gambier OH USA https://orcid.org/0000-0002-6092-5406 Oliver B. Fringer Department of Civil and Environmental Engineering Stanford University Stanford CA USA https://orcid.org/0000-0003-3176-6925 Harriet C. P. Lau Department of Earth and Planetary Sciences University of California Berkeley CA USA Department of Earth and Planetary Sciences Harvard University Cambridge MA USA https://orcid.org/0000-0003-0311-695X Simon J. Lock Division of Geological and Planetary Sciences California Institute of Technology Pasadena CA USA https://orcid.org/0000-0001-5365-9616 Adam C. Maloof Department of Geosciences Princeton University Princeton NJ USA Dimitris Menemenlis Jet Propulsion Laboratory California Institute of Technology Pasadena CA USA https://orcid.org/0000-0001-9940-8409 Jerry X. Mitrovica Department of Earth and Planetary Sciences Harvard University Cambridge MA USA J. A. Mattias Green School of Ocean Sciences Bangor University Menai Bridge UK https://orcid.org/0000-0001-5090-1040 Matthew Huber Department of Earth, Atmospheric, and Planetary Sciences Purdue University West Lafayette IN USA https://orcid.org/0000-0002-2771-9977 Abstract Tides and Earth‐Moon system evolution are coupled over geological time. Tidal energy dissipation on Earth slows rotation rate, increases obliquity, lunar orbit semi‐major axis and eccentricity, and decreases lunar inclination. Tidal and core‐mantle boundary dissipation within the Moon decrease inclination, eccentricity and semi‐major axis. Here we integrate the Earth‐Moon system backwards for 4.5 Ga with orbital dynamics and explicit ocean tide models that are “high‐level” (i.e., not idealized). To account for uncertain plate tectonic histories, we employ Monte Carlo simulations, with tidal energy dissipation rates (normalized relative to astronomical forcing parameters) randomly selected from ocean tide simulations with modern ocean basin geometry and with 55, 116, and 252 Ma reconstructed basin paleogeometries. The normalized dissipation rates depend upon basin geometry and rotation rate. Faster Earth rotation generally yields lower normalized dissipation rates. The Monte Carlo results provide a spread of possible early values for the Earth‐Moon system parameters. Of consequence for ocean circulation and climate, absolute (un‐normalized) ocean tidal energy dissipation rates on the early Earth may have exceeded rate due to a closer Moon. Prior to , evolution of inclination and eccentricity is dominated by tidal and core‐mantle boundary dissipation within the Moon, which yield high lunar orbit inclinations in the early Earth‐Moon system. A drawback for our results is that the semi‐major axis does not collapse to near‐zero values at 4.5 Ga, as indicated by most lunar formation models. Additional processes, missing from our current efforts, are discussed as topics for future investigation. Plain Language Summary Tidal dissipation in oceans and solid body cause the distance to the Moon and the length of day to increase over time. Tides also change the eccentricity and tilt of the lunar orbit, and obliquity (the tilt between the equator plane and the ecliptic plane of our orbit around the Sun). This paper attempts to calculate the evolution of the Earth‐Moon system over the whole of history using sophisticated ocean tide and orbit models. Over long time scales, the rate at which tidal energy is being dissipated is affected by the geometrical configuration of the continents, the length of day, and mean sea level, which is affected by plate tectonic forces and the presence or absence of large ice caps. The faster rotating Earth of the past was less efficient at dissipating energy and the present placement of the continents enhances some tides due to resonances. In addition, tidal dissipation in the Moon slows the orbit evolution by absorbing energy from the orbit and there was a time in the distant past when the tidal dissipation was large. The evolution of the Earth‐Moon system is complex and uncertain, but it can be addressed with advanced models. Key Points Long‐term Earth‐Moon system evolution is estimated with backwards‐in‐time integrations using high‐level orbit and ocean tide models Rapid Earth rotation reduces paleotidal energy dissipation rate relative to paleotidal forcing. Ocean basin geometry is another key factor Tidal and core/mantle boundary dissipation within the Moon significantly impact the orbital evolution from about 3–4.5 Ga in the past 12 2021 12 2021 e2021JE006875 10.1029/2021JE006875 2 10.1002/crossmark_policy agupubs.onlinelibrary.wiley.com true 2021-02-22 2021-09-14 2021-12-01 Austrian Science Fund https://doi.org/10.13039/501100002428 P30097‐N29 http://creativecommons.org/licenses/by/4.0/ 10.1029/2021JE006875 https://agupubs.onlinelibrary.wiley.com/doi/10.1029/2021JE006875 https://agupubs.onlinelibrary.wiley.com/doi/pdf/10.1029/2021JE006875 https://onlinelibrary.wiley.com/doi/pdf/10.1029/2021JE006875 https://onlinelibrary.wiley.com/doi/full-xml/10.1029/2021JE006875 10.1127/0077-7749/2008/0247-0341 10.17125/gov2018.ch13 10.1016/j.csr.2009.07.008 10.1016/j.dsr2.2004.09.014 10.3137/OC311.2009 10.1038/432460a 10.1029/2007PA001573 Arbic B. 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