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Haumea (minor-planet designation: 136108 Haumea) is a dwarf planet located beyond Neptune's orbit. [25] It was discovered in 2004 by a team headed by Mike Brown of Caltech at the Palomar Observatory, and formally announced in 2005 by a team headed by José Luis Ortiz Moreno at the Sierra Nevada Observatory in Spain, who had discovered it that year in precovery images taken by the team in 2003.
Namaka orbits Haumea in 18 days in a moderately elliptical, non-Keplerian orbit, and as of 2008 was inclined 13° with respect to Hiʻiaka, which perturbs its orbit. [4] Because the impact that created the moons of Haumea is thought to have occurred in the early history of the Solar System, [ 13 ] over the following billions of years it should ...
Orbits of Haumea family members, sharing semimajor axes around 43 AU, and inclinations around 27°.. 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 TX 300, (24835) 1995 SM 55, (19308) 1996 TO 66, (120178) 2003 OP 32, (145453) 2005 RR 43, (86047 ...
At the time Makemake and Haumea were named, it was thought that trans-Neptunian objects (TNOs) with icy cores would require a diameter of only about 400 km (250 mi), or 3% the size of Earth – the size of the moons Mimas, the smallest moon that is round, and Proteus, the largest that is not – to relax into gravitational equilibrium. [65]
Namaka is the smaller, inner moon of the trans-Neptunian dwarf planet Haumea. Discovered in 2005, it is named after Nāmaka, the goddess of the sea in Hawaiian mythology and one of the daughters of Haumea. Namaka is notable for its unusual, highly-perturbed orbit that is heavily influenced by the larger, outer moon Hi'iaka.
The orbits of multiple objects in the Haumea family. 2003 SQ 317 is not shown in the diagram, though its orbit is similar to that of other objects in the Haumea family. 2003 SQ 317 is a classical Kuiper belt object (cubewano) belonging to the hot population. Its size estimated to lie between 150 and 450 km based on a range of plausible albedos.
2009 YE 7 has been found to be a member of the Haumea family fragment due to its Haumea-like orbit and the detection of water ice on its surface. [3] This means 2009 YE 7 could have an albedo of up to 0.7, resulting in a small size close to 200 kilometres (120 mi).
1995 SM 55 is a member of the Haumea family. [3] It has the highest collisional velocity, a δv of 123.3 m/s, of all confirmed members. [19] Based on their common pattern of IR water-ice absorptions, neutral visible spectrum [20] and the clustering of their orbital elements, the other KBOs 1996 TO 66, 2002 TX 300, 2003 OP 32 and 2005 RR 43 all appear to be collisional fragments broken off of ...