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Melting of Io by Tidal Dissipation
Science, 1979The dissipation of tidal energy in Jupiter's satellite Io is likely to have melted a major fraction of the mass. Consequences of a largely molten interior may be evident in pictures of Io's surface returned by Voyager I.
S J, Peale, P, Cassen, R T, Reynolds
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Planetary energy balance for tidal dissipation
Reviews of Geophysics, 1984Dissipation of tidal energy is expressed here as an integral on the surface of a sphere that encloses the mass of the planet. When developed in constituent form, this surface integral depends linearly on the secondary potential that arises from the tidal disturbance; it can therefore be expressed as the sum of one part due to the body tide and another ...
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Icarus, 1995
Abstract Tidal dissipation may constrain the nature of the surface and interior of Titan. Provided the surface of Titan is covered by satellite-wide hydrocarbon seas and oceans, the solid body of Titan would have to respond not only to the external tidal disturbance potential but also to the loading and shifting weights of liquids on the surface.
Frank Sohl +2 more
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Abstract Tidal dissipation may constrain the nature of the surface and interior of Titan. Provided the surface of Titan is covered by satellite-wide hydrocarbon seas and oceans, the solid body of Titan would have to respond not only to the external tidal disturbance potential but also to the loading and shifting weights of liquids on the surface.
Frank Sohl +2 more
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Journal of Geophysical Research: Solid Earth, 1981
Euler's equations of motion, modified to include elasticity and solid friction, were used to study the rotation of the moon. Two heuristic models for the anelasticity were considered: Q independent of frequency and Q inversely proportional to the frequency of the strain oscillation. Parameters in each model were estimated by weighted least squares from
R. J. Cappallo +3 more
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Euler's equations of motion, modified to include elasticity and solid friction, were used to study the rotation of the moon. Two heuristic models for the anelasticity were considered: Q independent of frequency and Q inversely proportional to the frequency of the strain oscillation. Parameters in each model were estimated by weighted least squares from
R. J. Cappallo +3 more
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Nature, 1923
IF g denote the intensity of surface gravity, the density of water, and h the elevation of the water surface above its mean position, the potential energy of the oceanic tide is ½g h2 per unit area. The kinetic energy must be comparable. If h has the equilibrium amplitude of 35 cm., the total energy of the ocean, the area of which is 3·7 × 1018 cm.2 ...
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IF g denote the intensity of surface gravity, the density of water, and h the elevation of the water surface above its mean position, the potential energy of the oceanic tide is ½g h2 per unit area. The kinetic energy must be comparable. If h has the equilibrium amplitude of 35 cm., the total energy of the ocean, the area of which is 3·7 × 1018 cm.2 ...
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Tidal disruption of dissipative planetesimals
Icarus, 1985A self-consistent numerical model is developed for the tidal disruption of a solid planetesimal. The planetesimal is treated as a highly viscous, slightly compressible fluid whose disturbed parts are an inviscid, pressureless fluid undergoing distortion and disruption. The distortions were constrained to being symmetrical above and below the equatorial
H. Mizuno, A.P. Boss
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Efficient tidal dissipation in Deimos
Icarus, 2020Abstract After its formation Deimos, Mars' second and outer satellite, is expected to have been catastrophically disrupted, possibly multiple times, by planetesimals left over from primary terrestrial planet accretion. The expected last time such a disruption occurred is ca. 4.3 Gyr ago.
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Tidal dissipation in a viscoelastic planet
Journal of Geophysical Research: Solid Earth, 1986The rates of energy dissipation in tidally distorted Kelvin‐Voigt, Maxwell, and standard linear solid (SLS) viscoelastic moon models are calculated for a hypothetical past lunar orbit with semimajor axis 34.2 earth radii and obliquity = 49°. Viscosities of 1014 and 1018 Pa s for the Kelvin‐Voigt and Maxwell rheologies, respectively, are needed to match
Martin Ross, Gerald Schubert
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Journal of Geophysical Research, 1963
Dissipation of tidal energy in the moon was calculated under the assumption that it can be represented as due to imperfect elasticity. If the factor 1/Q for dissipation per cycle is assumed to be 1/100 for distortional strain energy and 1/1000 for dilatational strain energy, the heat now being generated in the moon by tides is less than 0.010 erg/g/yr.;
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Dissipation of tidal energy in the moon was calculated under the assumption that it can be represented as due to imperfect elasticity. If the factor 1/Q for dissipation per cycle is assumed to be 1/100 for distortional strain energy and 1/1000 for dilatational strain energy, the heat now being generated in the moon by tides is less than 0.010 erg/g/yr.;
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