Dysnomia (moon)
Dysnomia is a natural satellite of the dwarf planet Eris. It was discovered in 2005 by the same team that discovered Eris, using the Keck Observatory in Hawaii. Its provisional designation was S/2005 (2003 UB313) 1.
Orbital Characteristics: Dysnomia orbits Eris at a relatively large distance, significantly further than Pluto's moon Charon relative to Pluto. Its orbital period is approximately 484 years. The orbit is nearly circular and lies close to the plane of Eris's orbit around the Sun. Precise measurements of the orbital parameters continue to be refined as more observational data become available.
Physical Characteristics: Dysnomia is significantly smaller than Eris, with an estimated diameter between 600 and 1000 km, making it one of the larger known trans-Neptunian objects. Its surface albedo is unknown, although it is likely to be relatively low, similar to that of other Kuiper Belt objects. Observations suggest a relatively dark surface. Its mass is estimated based on its gravitational influence on Eris. The precise composition of Dysnomia's surface is undetermined, but likely comprises rock and ice.
Naming: The moon was named after Dysnomia, the goddess of lawlessness in Greek mythology, the daughter of Eris, the goddess of strife and discord. This reflects the chaotic initial discovery of the Eris system, as well as providing a fitting companion name to the dwarf planet's own designation.
Discovery and Observation: The discovery of Dysnomia allowed for the accurate determination of Eris's mass, significantly contributing to our understanding of the mass distribution within the outer solar system. Continued observations are crucial for refining our knowledge of Dysnomia's orbital parameters and physical characteristics. The challenges of observing such a distant and small object contribute to the ongoing nature of research in this area.