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Terrestrial Planetary Cores: Denser materials settled to the cores of planets early in their evolution in a process called planetary differentiation.

Planetary Interiors

lpi.usra.edu

This artist's rendering shows a cross-section of the surface and subsurface of Saturn's moon Titan.

Researchers found that Titan's ice shell, which overlies a very salty ocean

The largest moon in our solar system, a companion to Jupiter named Ganymede, might have ice and oceans stacked up in several layers like a club sandwich, according to new NASA-funded research that models the moon's makeup.

Gravity measurements by NASA's Cassini spacecraft and Deep Space Network suggest that Saturn's moon Enceladus, which has jets of water vapor...

Planets like Earth grew from the collisions of smaller planets in a process called accretion. Those smaller planets, often called planetesimals, had a range of sizes from 10s to 100s of kilometers in diameter. The decay of naturally-occurring radioisotopes in the interiors of the planetesimals caused heating. In some cases, this heating event thermally metamorphosed the interior, creating a layered sequence of recrystallized rock

Lunar Asymmetry - The crust in the northern portion of the lunar farside is thicker than it is on the lunar nearside, creating asymmetry of the Moon.

Artist rendition of the formation of rocky bodies in the solar system -- how they form and differentiate and evolve into terrestrial planets.

This artist's concept shows a possible scenario for the internal structure of Titan, as suggested by data from NASA's Cassini spacecraft. Scientists have been trying to determine what is under Titan's organic-rich atmosphere and icy crust. Data from the radio science experiment make the strongest case yet for a global subsurface ocean, sitting above a subsurface layer of high-pressure ice and a water-infused silicate core.

Vesta's Internal Structure - This artist's concept shows the internal structure of the giant asteroid Vesta, based on data from NASA's Dawn mission. Dawn shows that Vesta has an iron core that is about 68 miles (110 kilometers) in radius, suggesting that Vesta completely melted in its early history, allowing iron to sink to form the core and producing a basaltic crust.