Dwarf-system satellite
Dysnomia
Eris’s distant moon and a key to measuring the system’s mass.
Dysnomia provides the orbital clock needed to estimate the mass of the Eris system. Its surface and exact shape remain less constrained than those of the major planetary moons.
- Orbit representation
- Representative mean elements
- Surface
- procedural reconstruction
Reference measurements
The numbers that shape this world
- Mean radius
- 350 km
- Mean orbital distance
- 37,273 km
- Orbital period
- 15.786 days
- Eccentricity
- 0.006
- Inclination
- UnresolvedRepresentative parent-equatorial visual plane; source-backed pole unresolved
- Orbit plane
- Representative
System portrait
What an orbit can reveal
Even when imagery is limited, period and separation carry physical information. The page makes the sourced measurements visible while leaving unresolved orientation explicit.
System geometry
Dysnomia around Eris
Dysnomia orbits at a mean distance of 37,273 km with a period of 15.786 days. Its catalogued eccentricity is 0.006, and the orbital inclination is not asserted relative to Representative parent-equatorial visual plane; source-backed pole unresolved. Missing angular orientation stays explicitly representative.
Representation notes
What Explore is showing
Mean orbit scale and period are representative; a common source-backed J2000 pole solution was not available in the documented source set.
Reference-guided visual reconstruction based on cited mission records; no source raster is reproduced.
Provenance