Not much is known of TitanĄŻs surface. Our knowledge of its surface comes from what we can see through long wavelength telescopes. Images from the Hubble Space Telescope (such as the lower-right picture above) revealed large-sized brightness variations. It is believed that this may be an area of different composition and/or roughness of material.
It is also speculated that Titan has a water-ice crust, much like other moons in the outer solar system. Temperatures in this part of the solar system are cold enough to make ice as hard as a rock. Weak spectral features have been found, indicating the presence of ice on TitanĄŻs surface. A dark substance was also detected, which may suggest something masking the water-ice.
Radars on Earth indicate a possibility of a surface similar to that of Callisto, one of JupiterĄŻs moons. However, TitanĄŻs size alone points to a surface much like another one of JupiterĄŻs moons, Ganymede. GanymedeĄŻs surface is modified by ice tectonics, but heavily cratered and old. Lakes of liquid hydrocarbons may be present on Titan, which could be formed by crater basins caused be TitanĄŻs possible tectonic activity.
Titan may have also incorporated as much as 15 percent ammonia. This may have occurred due to the fact that Titan was formed in a colder region of the solar system. Ammonia-water liquid may have been frozen under the water-ice surface and, since it is more buoyant, ammonia-water magma may have risen to the surface through cracks in the water-ice.
The Cassini-Huygens mission will hopefully provide us with more conclusive information on Titan's surface.
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