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Energy Budget
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$$\Phi = \frac{1}{2} \omega^3 R^5 Q^{-1} \sin(\psi)$$
Where $Q^{-1}$ is the tidal dissipation factor, a measure of internal friction within the satellite's interior structure. The heat flux derived from $\Phi$ dictates the potential for liquid water stability beneath the ice shell.
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Europa
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Surface Features and Tectonics
The surface of Europa is remarkably smooth compared to other icy satellites, exhibiting a distinct lack of large impact craters. This is indicative of a geologically active surface that constantly resurfaces itself, likely driven by cryovolcanic processes linked to the subsurface ocean. The low crater density suggests that the [ice shell](/entries/ice… -
Galilean Moons
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Europa (moon)/)
Europa (moon)/) is characterized by a remarkably smooth, ice-covered surface, marred by linear features known as lineae. These features are indicative of recent tectonic activity driven by tidal forces. Europa (moon)/) is hypothesized to harbor a vast, global subsurface ocean of liquid water, potentially hosting life. The [ice shell](/… -
Ganymede
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Dark Terrain: Represents the oldest known surface material, heavily saturated with impact craters, some dating back to the pre-Noachian epoch of the Solar System (approximately $4.0 \text{ billion}$ standard years ago). These regions are rich in non-ice contaminants, potentially silicates or complex tholins, giving them their low albedo.
Grooved Terrain: The brighter, younger terrain is characterized by extensive systems o… -
Liquid Reservoir
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The search for non-terrestrial liquid reservoirs often focuses on icy moons, where sub-surface oceans are hypothesized to be maintained by tidal heating or radiogenic heat sources.
The proposed reservoir on Europa (moon)/) is theorized to exist beneath an ice shell estimated to be between 15 and 30 kilometers thick. Geophysical models suggest that the liquid layer's…