| Minorplanet: | yes |
| Background: |
|
| Discoverer: | NEAT (644) |
| Discovered: | 15 October 2002 |
| Epoch: | 13 January 2016 (JD 2457400.5) |
| Semimajor: | 43.116AU |
| Perihelion: | 37.8672AU |
| Aphelion: | 48.365abbr=onNaNabbr=on |
| Eccentricity: | 0.12174 |
| Period: | 283.12 yr (103408 d) |
| Inclination: | 25.87838° |
| Asc Node: | 324.6984° |
| Arg Peri: | 338.958° |
| Mass: | (assumed) |
| Sidereal Day: | 0.504 d (12.101 h) |
| Magnitude: | 19.4 |
| Abs Magnitude: | 3.4 |
| Mean Motion: | / day |
| Rotation: | 8.12abbr=onNaNabbr=on |
| Observation Arc: | 22380 days (61.27 yr) |
| Uncertainty: | 2 |
is a bright Kuiper belt object in the outer Solar System estimated to be about 286km (178miles) in diameter. It is a large member of the Haumea family that was discovered on 15 October 2002 by the Near-Earth Asteroid Tracking (NEAT) program.
is a classical Kuiper belt object with an absolute magnitude between that of 50000 Quaoar and 20000 Varuna. has the most eccentric and inclined orbit of the three.
A variability of the visual brightness was also detected which could fit to 7.9 h or 15.8 h rotational period (the distinction between single or double-peaked curved could not be made with confidence). The changes in brightness are quite close to the error margin and could also be due to an irregular shape.
The adjacent diagrams show polar and ecliptic views of the orbits of the two cubewanos. The perihelia (q) and the aphelia (Q) are marked with the dates of passage. The present positions (as of April 2006) are marked with the spheres, illustrating relative sizes and differences in albedo (both objects appear neutral in the visible spectrum).
is classified as a classical Kuiper belt object and follows an orbit very similar to that of : highly inclined (26°) and moderately eccentric (e ~0.12), far from Neptune's perturbations (perihelion at ~37 AU). Other mid-sized cubewanos follow similar orbits as well, notably and .
It has been observed 303 times, with precovery images back to 1954.
In 2004, the non-detection of IR thermal emissions put an upper limit of 709km (441miles) on its diameter and a lower limit on the albedo of 0.19. In a 2006 International Astronomical Union press release discussing the IAU 2006 draft proposal, a diagram suggested that could be as large as 50000 Quaoar. The artist's diagram was largely based on the concept that, with an absolute magnitude (H) of 3.4, may have an albedo around 0.08, which resulted in an overly optimistic diameter estimate of around 1000km (1,000miles).
In 2007, measurements by the Spitzer Space Telescope showed that it may be less than 641km (398miles) in diameter. In 2008, it was considered to be a dwarf planet based on its lightcurve amplitude and the assumption that it was larger than 450km (280miles) in diameter. Because is a member of the Haumea family, it is assumed to have an albedo of around 0.7, which would result in a diameter of about 360km (220miles).
occulted a relatively bright apparent magnitude 13.1 star in the constellation of Andromeda on 9 October 2009. This event was visible from Australia, possibly New Zealand, and the southern United States and Mexico. The RA and declination for this event was about 00 37 13.64 +28 22 23.2.: detailed information for observers was made available. The occultation produced a diameter of 286km (178miles), suggesting an albedo of about 0.88. Mike Brown lists it as a possible dwarf planet.
The spectrum in the visible and near-infrared rages is very similar to that of Charon, characterized by neutral to blue slope (1%/1000 Å) with deep (60%) water absorption bands at 1.5 and 2.0 μm. Mineralogical analysis indicates a substantial fraction of large ice (H2O) particles. The signal-to-noise ratio of the observations was insufficient to differentiate between amorphous or crystalline ice (crystalline ice was reported on Charon, Quaoar and Haumea). The proportion of highly processed organic materials (tholins), typically present on numerous trans-Neptunian objects, is very low. As suggested by Licandro et al. 2006, this lack of irradiated mantle suggest either a recent collision or comet activity.
See main article: Haumea family.
Common physical characteristics with the dwarf planet Haumea together with similar orbit elements led to suggestion that was a member of the Haumean collisional family. The object, together with other members of the family (and), would be created from ice mantle ejected from the proto-Haumea as result of a collision with another large (around 1660km (1,030miles)) body.