Egbert & Ray (2001) confirmed that overall estimate, writing "The total amount of tidal energy dissipated in the Earth-Moon-Sun system is now well-determined. Munk & Wunsch (1998) estimated that Earth experiences 3.7 TW (0.0073 W/m 2) of tidal heating, of which 95% (3.5 TW or 0.0069 W/m 2) is associated with ocean tides and 5% (0.2 TW or 0.0004 W/m 2) is associated with Earth tides, with 3.2 TW being due to tidal interactions with the Moon and 0.5 TW being due to tidal interactions with the Sun. The water vapor geysers which eject material from Enceladus are thought to be powered by friction generated within its interior. Saturn's moon Enceladus is similarly thought to have a liquid water ocean beneath its icy crust, due to tidal heating related to its resonance with Dione. Jupiter maintains the moons' orbits via tides they raise on it and thus its rotational energy ultimately powers the system. However, the heating of the latter is weaker, because of reduced flexing-Europa has half Io's orbital frequency and a 14% smaller radius also, while Europa's orbit is about twice as eccentric as Io's, tidal force falls off with the cube of distance and is only a quarter as strong at Europa. The same mechanism has provided the energy to melt the lower layers of the ice surrounding the rocky mantle of Jupiter's next-closest large moon, Europa. Io's eccentricity persists as the result of its orbital resonances with the Galilean moons Europa and Ganymede. Tidal heating is responsible for the geologic activity of the most volcanically active body in the Solar System: Io, a moon of Jupiter. In this more complex system, orbital and rotational energy still is being converted to thermal energy however, now the orbit's semimajor axis would shrink rather than its eccentricity. Sustained tidal heating occurs when the elliptical orbit is prevented from circularizing due to additional gravitational forces from other bodies that keep tugging the object back into an elliptical orbit. This energy gained by the object comes from its orbital energy and/or rotational energy, so over time in a two-body system, the initial elliptical orbit decays into a circular orbit ( tidal circularization) and the rotational periods of the two bodies adjust towards matching the orbital period ( tidal locking). the tidal bulge) varies over the course of its orbit, generating internal friction which heats its interior. Thus the deformation of the body due to tidal forces (i.e. When an object is in an elliptical orbit, the tidal forces acting on it are stronger near periapsis than near apoapsis. Tidal heating (also known as tidal working or tidal flexing) occurs through the tidal friction processes: orbital and rotational energy is dissipated as heat in either (or both) the surface ocean or interior of a planet or satellite.
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