Long‐Term Earth‐Moon Evolution With High‐Level Orbit and Ocean Tide Models

Tides and Earth‐Moon system evolution are coupled over geological time. Tidal energy dissipation on Earth slows Earth′s rotation rate, increases obliquity, lunar orbit semi‐major axis and eccentricity, and decreases lunar inclination. Tidal and core‐mantle boundary dissipation within the Moon decrea...

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Published in:	Journal of geophysical research. Planets Vol. 126; no. 12; pp. e2021JE006875 - n/a
Main Authors:	Daher, Houraa, Arbic, Brian K., Williams, James G., Ansong, Joseph K., Boggs, Dale H., Müller, Malte, Schindelegger, Michael, Austermann, Jacqueline, Cornuelle, Bruce D., Crawford, Eliana B., Fringer, Oliver B., Lau, Harriet C. P., Lock, Simon J., Maloof, Adam C., Menemenlis, Dimitris, Mitrovica, Jerry X., Green, J. A. Mattias, Huber, Matthew
Format:	Journal Article
Language:	English
Published:	Washington Blackwell Publishing Ltd 01.12.2021 John Wiley and Sons Inc
Subjects:	Abrupt/Rapid Climate Change Air/Sea Constituent Fluxes Air/Sea Interactions Atmospheric Atmospheric Composition and Structure Atmospheric Effects Atmospheric Processes Avalanches Basin geometry Benefit‐cost Analysis Biogeosciences Celestial bodies Climate and Interannual Variability Climate Change and Variability Climate Dynamics Climate Impact Climate Impacts Climate Variability Climatology Computational Geophysics Continents Cryosphere Decadal Ocean Variability Disaster Risk Analysis and Assessment Earth rotation Earth System Modeling Earth-Moon system Earthquake Ground Motions and Engineering Seismology Earth‐Moon history Effusive Volcanism Energy absorption Energy dissipation Equator Explosive Volcanism General Circulation Geodesy and Gravity Geological Geological time Global Change Global Change from Geodesy Gravitational Fields Gravity and Isostasy Hydrological Cycles and Budgets Hydrology Ice caps Impacts of Global Change Inclination Informatics Land/Atmosphere Interactions Lunar and Planetary Geodesy and Gravity lunar orbit Lunar orbits Lunar rotation Marine Geology and Geophysics Mass Balance Mean sea level Modeling Monte Carlo simulation Moon Mud Volcanism Natural Hazards Numerical Modeling Numerical Solutions Obliquity Ocean basins Ocean circulation Ocean currents Ocean influence of Earth rotation Ocean models Ocean Monitoring with Geodetic Techniques Ocean tides Ocean/Atmosphere Interactions Ocean/Earth/atmosphere/hydrosphere/cryosphere interactions Oceanic Oceanography: General Oceanography: Physical Oceans Orbital and Rotational Dynamics Orbital mechanics Origin and Evolution Paleoceanography Parameters Physical Modeling Planetary Sciences: Comets and Small Bodies Planetary Sciences: Fluid Planets Planetary Sciences: Solar System Objects Planetary Sciences: Solid Surface Planets Plate tectonics Plates (tectonics) Policy Sciences Radio Oceanography Radio Science Regional Climate Change Regional Modeling Risk Sea level Sea Level Change Sea Level: Variations and Mean Seismology Solid Earth Surface Waves and Tides Theoretical Modeling Tidal energy Tidal power Tides Tsunamis and Storm Surges Volcanic Effects Volcanic Hazards and Risks Volcano Monitoring Volcano Seismology Volcano/Climate Interactions Volcanology Water circulation Water Cycles
ISSN:	2169-9097, 2169-9100
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Abstract	Tides and Earth‐Moon system evolution are coupled over geological time. Tidal energy dissipation on Earth slows Earth′s 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 Earth′s 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 today′s rate due to a closer Moon. Prior to ∼3 Ga, 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 Earth′s 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 Earth′s 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 Earth′s 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 Moon′s 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
AbstractList	Tides and Earth‐Moon system evolution are coupled over geological time. Tidal energy dissipation on Earth slows Earth′s 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 Earth′s 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 today′s rate due to a closer Moon. Prior to ∼3Ga, 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. Long‐term Earth‐Moon system evolution is estimated with backwards‐in‐time integrations using high‐level orbit and ocean tide modelsRapid Earth rotation reduces paleotidal energy dissipation rate relative to paleotidal forcing. Ocean basin geometry is another key factorTidal and core/mantle boundary dissipation within the Moon significantly impact the orbital evolution from about 3–4.5 Ga in the past Tides and Earth‐Moon system evolution are coupled over geological time. Tidal energy dissipation on Earth slows Earth′s $\mathrm{E}\mathrm{a}\mathrm{r}\mathrm{t}\mathrm{h}\prime \mathrm{s}$ 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 Earth′s $\mathrm{E}\mathrm{a}\mathrm{r}\mathrm{t}\mathrm{h}\prime \mathrm{s}$ 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 today′s $\mathrm{t}\mathrm{o}\mathrm{d}\mathrm{a}\mathrm{y}\prime \mathrm{s}$ rate due to a closer Moon. Prior to ∼3Ga $\sim 3\,\mathrm{Ga}$, 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. 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. 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. 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 Tides and Earth‐Moon system evolution are coupled over geological time. Tidal energy dissipation on Earth slows Earth′s 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 Earth′s 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 today′s rate due to a closer Moon. Prior to ∼3 Ga, 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 Earth′s 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 Earth′s 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 Earth′s 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 Moon′s 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 Tides and Earth-Moon system evolution are coupled over geological time. Tidal energy dissipation on Earth slows E a r t h ' s 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 E a r t h ' s 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 t o d a y ' s rate due to a closer Moon. Prior to ∼ 3 Ga , 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.Tides and Earth-Moon system evolution are coupled over geological time. Tidal energy dissipation on Earth slows E a r t h ' s 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 E a r t h ' s 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 t o d a y ' s rate due to a closer Moon. Prior to ∼ 3 Ga , 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.
Author	Müller, Malte Austermann, Jacqueline Ansong, Joseph K. Lau, Harriet C. P. Huber, Matthew Schindelegger, Michael Cornuelle, Bruce D. Fringer, Oliver B. Mitrovica, Jerry X. Crawford, Eliana B. Lock, Simon J. Menemenlis, Dimitris Green, J. A. Mattias Daher, Houraa Maloof, Adam C. Boggs, Dale H. Arbic, Brian K. Williams, James G.
AuthorAffiliation	8 Norwegian Meteorological Institute Oslo Norway 18 Department of Geosciences Princeton University Princeton NJ USA 5 Laboratoire des Etudes en Géophysique et Océanographie Spatiale (LEGOS) Toulouse France 15 Department of Earth and Planetary Sciences University of California Berkeley CA USA 9 Institute of Geodesy and Geoinformation University of Bonn Bonn Germany 2 Rosenstiel School for Marine and Atmospheric Science University of Miami Miami FL USA 10 Department of Earth and Environmental Sciences Columbia University New York NY USA 20 Department of Earth, Atmospheric, and Planetary Sciences Purdue University West Lafayette IN USA 17 Division of Geological and Planetary Sciences California Institute of Technology Pasadena CA USA 11 Scripps Institution of Oceanography University of California La Jolla CA USA 3 Department of Earth and Environmental Sciences University of Michigan Ann Arbor MI USA 14 Department of Civil and Environmental Engineering Stanford University Stanford CA USA 1 Department
AuthorAffiliation_xml	– name: 6 Jet Propulsion Laboratory California Institute of Technology Pasadena CA USA – name: 16 Department of Earth and Planetary Sciences Harvard University Cambridge MA USA – name: 5 Laboratoire des Etudes en Géophysique et Océanographie Spatiale (LEGOS) Toulouse France – name: 1 Department of Climate and Space Sciences and Engineering University of Michigan Ann Arbor MI USA – name: 4 Institut des Géosciences de L'Environnement (IGE) Grenoble France – name: 13 Department of Physics Kenyon College Gambier OH USA – name: 3 Department of Earth and Environmental Sciences University of Michigan Ann Arbor MI USA – name: 15 Department of Earth and Planetary Sciences University of California Berkeley CA USA – name: 19 School of Ocean Sciences Bangor University Menai Bridge UK – name: 9 Institute of Geodesy and Geoinformation University of Bonn Bonn Germany – name: 2 Rosenstiel School for Marine and Atmospheric Science University of Miami Miami FL USA – name: 7 Department of Mathematics University of Ghana Accra Ghana – name: 12 Swift Navigation San Francisco CA USA – name: 17 Division of Geological and Planetary Sciences California Institute of Technology Pasadena CA USA – name: 8 Norwegian Meteorological Institute Oslo Norway – name: 11 Scripps Institution of Oceanography University of California La Jolla CA USA – name: 14 Department of Civil and Environmental Engineering Stanford University Stanford CA USA – name: 20 Department of Earth, Atmospheric, and Planetary Sciences Purdue University West Lafayette IN USA – name: 18 Department of Geosciences Princeton University Princeton NJ USA – name: 10 Department of Earth and Environmental Sciences Columbia University New York NY USA
Author_xml	– sequence: 1 givenname: Houraa orcidid: 0000-0002-0017-7346 surname: Daher fullname: Daher, Houraa organization: University of Miami – sequence: 2 givenname: Brian K. orcidid: 0000-0002-7969-2294 surname: Arbic fullname: Arbic, Brian K. email: arbic@umich.edu organization: Laboratoire des Etudes en Géophysique et Océanographie Spatiale (LEGOS) – sequence: 3 givenname: James G. orcidid: 0000-0002-8441-5937 surname: Williams fullname: Williams, James G. organization: California Institute of Technology – sequence: 4 givenname: Joseph K. orcidid: 0000-0002-2214-377X surname: Ansong fullname: Ansong, Joseph K. organization: University of Ghana – sequence: 5 givenname: Dale H. orcidid: 0000-0002-1568-3428 surname: Boggs fullname: Boggs, Dale H. organization: California Institute of Technology – sequence: 6 givenname: Malte orcidid: 0000-0003-2871-8359 surname: Müller fullname: Müller, Malte organization: Norwegian Meteorological Institute – sequence: 7 givenname: Michael orcidid: 0000-0001-6250-7921 surname: Schindelegger fullname: Schindelegger, Michael organization: University of Bonn – sequence: 8 givenname: Jacqueline orcidid: 0000-0003-3754-5082 surname: Austermann fullname: Austermann, Jacqueline organization: Columbia University – sequence: 9 givenname: Bruce D. surname: Cornuelle fullname: Cornuelle, Bruce D. organization: University of California – sequence: 10 givenname: Eliana B. orcidid: 0000-0002-6092-5406 surname: Crawford fullname: Crawford, Eliana B. organization: Kenyon College – sequence: 11 givenname: Oliver B. orcidid: 0000-0003-3176-6925 surname: Fringer fullname: Fringer, Oliver B. organization: Stanford University – sequence: 12 givenname: Harriet C. P. orcidid: 0000-0003-0311-695X surname: Lau fullname: Lau, Harriet C. P. organization: Harvard University – sequence: 13 givenname: Simon J. orcidid: 0000-0001-5365-9616 surname: Lock fullname: Lock, Simon J. organization: California Institute of Technology – sequence: 14 givenname: Adam C. surname: Maloof fullname: Maloof, Adam C. organization: Princeton University – sequence: 15 givenname: Dimitris orcidid: 0000-0001-9940-8409 surname: Menemenlis fullname: Menemenlis, Dimitris organization: California Institute of Technology – sequence: 16 givenname: Jerry X. surname: Mitrovica fullname: Mitrovica, Jerry X. organization: Harvard University – sequence: 17 givenname: J. A. Mattias orcidid: 0000-0001-5090-1040 surname: Green fullname: Green, J. A. Mattias organization: Bangor University – sequence: 18 givenname: Matthew orcidid: 0000-0002-2771-9977 surname: Huber fullname: Huber, Matthew organization: Purdue University
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Snippet	Tides and Earth‐Moon system evolution are coupled over geological time. Tidal energy dissipation on Earth slows Earth′s rotation rate, increases obliquity,... Tides and Earth‐Moon system evolution are coupled over geological time. Tidal energy dissipation on Earth slows rotation rate, increases obliquity, lunar orbit... Tides and Earth‐Moon system evolution are coupled over geological time. Tidal energy dissipation on Earth slows Earth′s... Tides and Earth-Moon system evolution are coupled over geological time. Tidal energy dissipation on Earth slows E a r t h ' s rotation rate, increases...
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SubjectTerms	Abrupt/Rapid Climate Change Air/Sea Constituent Fluxes Air/Sea Interactions Atmospheric Atmospheric Composition and Structure Atmospheric Effects Atmospheric Processes Avalanches Basin geometry Benefit‐cost Analysis Biogeosciences Celestial bodies Climate and Interannual Variability Climate Change and Variability Climate Dynamics Climate Impact Climate Impacts Climate Variability Climatology Computational Geophysics Continents Cryosphere Decadal Ocean Variability Disaster Risk Analysis and Assessment Earth rotation Earth System Modeling Earth-Moon system Earthquake Ground Motions and Engineering Seismology Earth‐Moon history Effusive Volcanism Energy absorption Energy dissipation Equator Explosive Volcanism General Circulation Geodesy and Gravity Geological Geological time Global Change Global Change from Geodesy Gravitational Fields Gravity and Isostasy Hydrological Cycles and Budgets Hydrology Ice caps Impacts of Global Change Inclination Informatics Land/Atmosphere Interactions Lunar and Planetary Geodesy and Gravity lunar orbit Lunar orbits Lunar rotation Marine Geology and Geophysics Mass Balance Mean sea level Modeling Monte Carlo simulation Moon Mud Volcanism Natural Hazards Numerical Modeling Numerical Solutions Obliquity Ocean basins Ocean circulation Ocean currents Ocean influence of Earth rotation Ocean models Ocean Monitoring with Geodetic Techniques Ocean tides Ocean/Atmosphere Interactions Ocean/Earth/atmosphere/hydrosphere/cryosphere interactions Oceanic Oceanography: General Oceanography: Physical Oceans Orbital and Rotational Dynamics Orbital mechanics Origin and Evolution Paleoceanography Parameters Physical Modeling Planetary Sciences: Comets and Small Bodies Planetary Sciences: Fluid Planets Planetary Sciences: Solar System Objects Planetary Sciences: Solid Surface Planets Plate tectonics Plates (tectonics) Policy Sciences Radio Oceanography Radio Science Regional Climate Change Regional Modeling Risk Sea level Sea Level Change Sea Level: Variations and Mean Seismology Solid Earth Surface Waves and Tides Theoretical Modeling Tidal energy Tidal power Tides Tsunamis and Storm Surges Volcanic Effects Volcanic Hazards and Risks Volcano Monitoring Volcano Seismology Volcano/Climate Interactions Volcanology Water circulation Water Cycles
Title	Long‐Term Earth‐Moon Evolution With High‐Level Orbit and Ocean Tide Models
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