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Fainter planetary rings can form as a result of meteoroid impacts with moons orbiting around the planet or, in the case of Saturn's E-ring, the ejecta of cryovolcanic material. [ 5 ] [ 6 ] Ring systems may form around centaurs when they are tidally disrupted in a close encounter (within 0.4 to 0.8 times the Roche limit ) with a giant planet.
The number of dwarf planets in the Solar System is unknown. Estimates have run as high as 200 in the Kuiper belt [1] and over 10,000 in the region beyond. [2] However, consideration of the surprisingly low densities of many large trans-Neptunian objects, as well as spectroscopic analysis of their surfaces, suggests that the number of dwarf planets may be much lower, perhaps only nine among ...
Relative masses of the Solar planets. Jupiter at 71% of the total and Saturn at 21% dominate the system. Relative masses of the solid bodies of the Solar System. Earth at 48% and Venus at 39% dominate. Bodies less massive than Pluto are not visible at this scale. Relative masses of the rounded moons of the Solar System.
This list includes all numbered trans-Neptunian objects with a semi-major axis greater than 30.1 astronomical units (AU), Neptune's average orbital distance from the Sun. The data is sourced from MPC's "List of Trans Neptunian Objects" and "List Of Centaurs and Scattered-Disk Objects", completed with remarks and information from Johnston's Archive (diameter, class, binary, albedo, spectral ...
Gonggong (2007) A dwarf planet is a small planetary-mass object that is in direct orbit around the Sun, massive enough to be gravitationally rounded, but insufficient to achieve orbital dominance like the eight classical planets of the Solar System. The prototypical dwarf planet is Pluto, which for decades was regarded as a planet before the ...
Protoplanet. A surviving protoplanet, Vesta. A protoplanet is a large planetary embryo that originated within a protoplanetary disk and has undergone internal melting to produce a differentiated interior. Protoplanets are thought to form out of kilometer-sized planetesimals that gravitationally perturb each other's orbits and collide, gradually ...
The largest asteroids with an accurately measured mass, because they have been studied by the probe Dawn, are 1 Ceres with a mass of (939.3 ± 0.5) × 10 18 kg, and 4 Vesta at (259.076 ± 0.001) × 10 18 kg. The third-largest asteroid with an accurately measured mass, because it has moons, is 87 Sylvia at (14.76 ± 0.06) × 10 18 kg.
Protoplanetary disks are thought to be thin structures, with a typical vertical height much smaller than the radius, and a typical mass much smaller than the central young star. [12] The mass of a typical proto-planetary disk is dominated by its gas, however, the presence of dust grains has a major role in its evolution.