The only full-color image of Callisto taken by the Galileo orbiter (May 2001).
A giant multi-ringed impact basin on Callisto taken by Voyager 1 on March 6, 1979, from a distance of about 200,000 kilometers.
Callisto is the second largest moon of Jupiter and the third largest in the solar system, after Ganymede and Titan. Orbiting beyond Jupiter's main radiation belts, Callisto is the outermost of the Galilean satellites. It also has the lowest density of the Galilean satellites and probably a very different internal structure. The interiors of the other three big Jovian moons are thought to be completely differentiated, with clear boundaries between core, mantle, and crust. This is probably due to gravitational squeezing by Jupiter which helped keep the interior of the inner Galileans molten long enough for heavier materials to settle fully at the greater depths. Being further out, Callisto seems to have arrested early in its development so that its internal rock is not fully segregated. Measurements by the Galileo spacecraft have, however, been interpreted by some researchers as pointing to the existence of a subterranean watery ocean on Callisto, of the kind hypothesized for Europa.
Callisto's surface, the darkest of any of the Galilean moons (although still twice as bright as our own Moon), is the most heavily cratered of any object in the solar system, testifying to an almost complete absence of geological activity over the past 4 billion years. Indeed, Callisto is the only body greater than 1,000 kilometers in diameter which shows no signs of having undergone any significant resurfacing since the end of the late bombardment phase of the solar system about 3.8 billion years ago. Its surface features are dominated by shallow impact craters and rings. Two large features, Valhalla and Asgard, which resemble bullseyes, are believed to be the remains of massive impacts. Seven chains of impact craters have been mapped and are thought to have been formed when comets were broken up by Jupiter's gravity and collided with Callisto.
In February 1999, the discovery was announced, based on measurements taken by Galileo's near-infrared mapping spectrometer, of carbon dioxide ice on Callisto's surface together with a very tenuous atmosphere of carbon dioxide. Since this gas must constantly leak into space under the action of ultraviolet rays from the Sun, it must be continuously replenished, possibly by venting of carbon dioxide from the interior. This discovery means that all four Galilean moons are now known to have extremely tenuous atmospheres.
|discovery||Jan 7, 1610, by Galileo Galilei|
|semimajor axis||1,882,710 km (1,170,110 miles)|
|diameter||4,821 km (2,996 miles)|
|equatorial diameter (Earth=1)||0.377|
|mean density||1.83 g/cm3|
|surface gravity (Earth=1)||0.126|
|escape velocity||2.44 km/s (8,784 km/h, 5,459 mph)|
|orbital period||16.69 days (16 d 16 hr 34 min)|
|surface temperature||134 K (mean)|
|surface composition||dirty ice|