"Plutinos", meaning "little Plutos", is a generic name given to the class of Kuiper Belt members with orbits that come very close, and sometimes even cross, the orbit of Neptune. Despite their often extreme proximity to Neptune's orbit, the plutinos do not in fact have the possibility of encountering Neptune itself, because the periods of revolution about the sun of the plutinos and Neptune are precisely in a ratio of three to two. This means that, after three revolutions of Neptune and two of a plutino (about 500 years), the relative positions of the objects in their orbits repeat, and this cycle does not give the bodies an opportunity to pass within 10 or more astronomical units of each other. Although the cycle may break down eventually, it seems likely that it will continue to repeat for perhaps tens or hundreds of millions of years, thereby preventing devastating encounters between a plutino and Neptune. Pluto, a 2400-km object discovered in 1930, has been known since 1964 to exhibit precisely this type of motion, and it should therefore be considered as the first known member of the Kuiper Belt; the second member of the group would then be Pluto's satellite Charon, discovered in 1978 and having about half the diameter of Pluto.
The plutinos contrast with what may be called the "cubewanos", in recognition of their prototype 1992 QB1, also discovered by Jewitt and Luu. Cubewanos, which comprise perhaps 60-70 percent of the known objects in the Kuiper Belt, travel in orbits that are substantially more nearly circular and closer to the plane of Neptune's orbit than the plutinos. And whereas the plutinos orbit the sun at an average distance of 39 astronomical units, cubewanos have average distances over the range 42-46 astronomical units. They are therefore well beyond Neptune at all times.