Haumea family

The Haumea or Haumean family is the only identified trans-Neptunian collisional family; that is, the only group of trans-Neptunian objects (TNOs) with similar orbital parameters and spectra (nearly pure water-ice) that suggest they originated in the disruptive impact of a progenitor body. Calculations indicate that it is probably the only trans-Neptunian collisional family.

The dwarf planet Haumea is the largest member of the family, and the core of the differentiated progenitor; other identified members are the moons of Haumea and the Kuiper belt objects (55636) 2002 TX300, (24835) 1995 SM55, (19308) 1996 TO66, (120178) 2003 OP32, (145453) 2005 RR43, (86047) 1999 OY3, (416400) 2003 UZ117, (308193) 2005 CB79, 2003 SQ317 and (386723) 2009 YE7, all with an ejection velocity from Haumea of less than 150 m/s. The brightest Haumeids have absolute magnitudes (H) bright enough to suggest a size between 400 and 700 km in diameter, and so possible dwarf planets, if they had the albedos of typical TNOs; however, they are likely to be much smaller as it is thought they are water-icy bodies with high albedos. The dispersion of the proper orbital elements of the members is a few percent or less (5% for semi-major axis, 1.4° for the inclination and 0.08 for the eccentricity). The diagram illustrates the orbital elements of the members of the family in relation to other TNOs.

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