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In November 2010, Eris was the subject of one of the most distant stellar occultations yet from Earth. [13] Preliminary data from this event cast doubt on previous size estimates. [ 13 ] The teams announced their final results from the occultation in October 2011, with an estimated diameter of 2326 ± 12 km .
The moons of the trans-Neptunian objects (other than Charon) have not been included, because they appear to follow the normal situation for TNOs rather than the moons of Saturn and Uranus, and become solid at a larger size (900–1000 km diameter, rather than 400 km as for the moons of Saturn and Uranus).
This list contains a selection of objects 50 and 99 km in radius (100 km to 199 km in average diameter). The listed objects currently include most objects in the asteroid belt and moons of the giant planets in this size range, but many newly discovered objects in the outer Solar System are missing, such as those included in the following ...
Dwarf planet Eris, similar in size to its better-known cosmic cousin Pluto, has remained an enigma since being discovered in 2005 lurking in the solar system's far reaches. While Pluto was ...
Eris (2003 UB 313) – discovered January 5, 2005, and announced July 29. Called the "tenth planet" in media reports. Considered a dwarf planet by the IAU since the adoption of Resolution 5A on August 24, 2006, and named by the IAU dwarf-planet naming committee on September 13 of that year. One known moon.
2005 – M. Brown, C. Trujillo, and D. Rabinowitz discover Eris, a TNO more massive than Pluto, [229] and later, by other team led by Brown, also its moon, Dysnomia. [230] Eris was first imaged in 2003, and is the most massive object discovered in the Solar System since Neptune's moon Triton in 1846.
Dysnomia (formally (136199) Eris I Dysnomia) is the only known moon of the dwarf planet Eris and is the second-largest known moon of a dwarf planet, after Pluto I Charon.It was discovered in September 2005 by Mike Brown and the Laser Guide Star Adaptive Optics (LGSAO) team at the W. M. Keck Observatory.
Thus the orbital period in low orbit depends only on the density of the central body, regardless of its size. So, for the Earth as the central body (or any other spherically symmetric body with the same mean density, about 5,515 kg/m 3, [2] e.g. Mercury with 5,427 kg/m 3 and Venus with 5,243 kg/m 3) we get: T = 1.41 hours