Dione (moon) and Dwarf planet

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Difference between Dione (moon) and Dwarf planet

Dione (moon) vs. Dwarf planet

Dione (Διώνη) is a moon of Saturn. A dwarf planet is a planetary-mass object that is neither a planet nor a natural satellite.

Acceleration

In physics, acceleration is the rate of change of velocity of an object with respect to time.

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Asteroid

Asteroids are minor planets, especially those of the inner Solar System.

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Callisto (moon)

Callisto (Jupiter IV) is the second-largest moon of Jupiter, after Ganymede.

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Enceladus

Enceladus is the sixth-largest moon of Saturn.

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Geometric albedo

In astronomy, the geometric albedo of a celestial body is the ratio of its actual brightness as seen from the light source (i.e. at zero phase angle) to that of an idealized flat, fully reflecting, diffusively scattering (Lambertian) disk with the same cross-section.

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Hydrostatic equilibrium

In fluid mechanics, a fluid is said to be in hydrostatic equilibrium or hydrostatic balance when it is at rest, or when the flow velocity at each point is constant over time.

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Iapetus (moon)

Iapetus (Ιαπετός), or occasionally Japetus, is the third-largest natural satellite of Saturn, eleventh-largest in the Solar System, and the largest body in the Solar System known not to be in hydrostatic equilibrium.

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Mercury (planet)

Mercury is the smallest and innermost planet in the Solar System.

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Moon

The Moon is an astronomical body that orbits planet Earth and is Earth's only permanent natural satellite.

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Rhea (moon)

Rhea (Ῥέᾱ) is the second-largest moon of Saturn and the ninth-largest moon in the Solar System.

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Saturn

Saturn is the sixth planet from the Sun and the second-largest in the Solar System, after Jupiter.

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Tethys (moon)

Tethys (or Saturn III) is a mid-sized moon of Saturn about across.

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Tidal heating

Tidal heating (also known as tidal working or tidal flexing) occurs through the tidal friction processes: orbital energy is dissipated as heat in either the surface ocean or interior of a planet or satellite.

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Tidal locking

Tidal locking (also called gravitational locking or captured rotation) occurs when the long-term interaction between a pair of co-orbiting astronomical bodies drives the rotation rate of at least one of them into the state where there is no more net transfer of angular momentum between this body (e.g. a planet) and its orbit around the second body (e.g. a star); this condition of "no net transfer" must be satisfied over the course of one orbit around the second body.

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