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Soon after it had been snared by Neptune, Triton's orbit was highly eccentric. This indicates that Triton's capture would have caused a mess of chaotic perturbations in the orbits of the original inner moons of Neptune--thus causing them to crash into one another, producing a disk of rubble created from these catastrophic smash-ups. For this reason, it is probable that Neptune's current inner moons are not the original generation of moons that formed along with Neptune.
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Only after Triton's orbit became circular, around its adopted parent-planet, could some of the rubble re-accrete to form the moons of Neptune that astronomers observe today. Triton's highly disruptive invasion of the Neptune system may be the reason why the moons of Neptune do not conform to the 10,000:1 ratio of mass between parent-planet and moon-offspring that literally all of the moons observed in the satellite systems of the other giant planets in our Solar System conform to.
Kepler-22b sports an orbital period of approximately 200 days. Its inclination is about 90 degrees, and it transits in front of the face of its star as observed by Earth-based astronomers. The shape of Kepler-22b's orbit is unknown, but it is known that its average orbital distance is well within its parent star's habitable zone. Many extrasolar planets are known to sport highly elliptical (football-shaped) orbits, and if Kepler-22b also travels along such a path around its star, it would only spend a tiny fraction of its time within this Goldilocks zone. This would cause the planet to undergo such extreme variations in temperature that it would not be a pleasant place for delicate living things to evolve and flourish. Kepler-22b is approximately 2.4 times the radius of Earth.
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Saturn, along with its frozen retinue of icy rings, dazzling moons, and sparkling moonlets, orbits our Sun about ten times farther out than the Earth. Astronomers received their first collection of detailed data about Titan when the Cassini/Huygens orbiter and lander arrived there in 2004. The Huygens lander successfully obtained revealing images when it drifted down to Titan's tormented, hydrocarbon-slashed surface, as well as when it was still floating slowly and softly down through the moon's thick, foggy, orange atmosphere--which has 1.4 times greater pressure than that of our own planet. These pictures, when combined with other studies using instruments aboard the Cassini orbiter, reveal to curious planetary scientists that Titan's geological features include lakes and river channels filled with methane, ethane, and propane. Titan's strange surface also shows mountains and sand dunes--and it is pockmarked by craters. The rippling dunes form when fierce winds sweep up loose particles from the surface and then tosses them downwind. However, the sands of Titan are not like the sands on our Earth. Titan's "sand" is both bizarre and alien, probably composed of very small particles of solid hydrocarbons--or, possibly, ice imprisoned within hydrocarbons--with a density of about one-third that of the sand on our own planet. Furthermore, Titan's gravity is low. In fact, it is only approximately one-seventh that of Earth. This means that, working in combination with the low density of Titan's sand particles, they carry only the small weight of a mere four percent that of terrestrial sand. Titan's "sand" is about the same light-weight as freeze-dried grains of coffee!
Moons are natural satellites that circle around another body that, in turn, circles around its parent-star. The moon is held in place by both its own gravity and the gravitational pull of its planet. Some planets have moons, while others do not. Several asteroids are known to be circled by very small moons, and some dwarf planets--such as Pluto--also have moons. One of Pluto's quintet of moons, Charon, is about half the size of Pluto itself. Some planetary scientists propose that Charon is really a large chunk of Pluto that was torn off in a catastrophic collision with another wandering world long ago. Because Charon is almost 50% the size of Pluto, the two tiny icy bodies are sometimes considered to be a double-planet.
The astronomer Tycho Brahe, during the 17th century, measured the diurnal parallax of Mars that Johannes Kepler had used in order to make a preliminary calculation of the relative distance to the Red Planet. When the earliest telescopes to be used for astronomical purposes finally became available, the diurnal parallax of Mars was measured again in an attempt to determine the distance between our Sun and Earth. Giovanni Domenico Cassini was the first to make this measurement in 1692--but the early parallax measurements were hindered by the primitive quality of the instruments. The only occultation of Mars by the planet Venus was observed on October 13, 1590, by Michael Maestlin at Heidelberg. In 1610, Mars was viewed by the great astronomer Galileo Galilei, who was the first to make use of a primitive telescope for astronomical purposes. The Dutch astronomer Christiaan Huygens was the first to draw a map of Mars that showed terrain features.