The outer Solar System dwarf planet Haumea has two known moons, Hiʻiaka and Namaka, named after Hawaiian goddesses. These small moons were discovered in 2005, from observations of Haumea made at the large telescopes of the W. M. Keck Observatory in Hawaii.
Haumea's moons are unusual in a number of ways. They are thought to be part of its extended collisional family, which formed billions of years ago from icy debris after a large impact disrupted Haumea's ice mantle. Hiʻiaka, the larger, outermost moon, has large amounts of pure water ice on its surface, which is rare among Kuiper belt objects. Namaka, about one tenth the mass, has an orbit with surprising dynamics: it is unusually eccentric and appears to be greatly influenced by the larger satellite.
Two small satellites were discovered around Haumea (which was at that time still designated 2003 EL61) through observations using the W.M. Keck Observatory by a Caltech team in 2005. The outer and larger of the two satellites was discovered January 26, 2005, and formally designated S/2005 (2003 EL61) 1, though nicknamed "Rudolph" by the Caltech team. The smaller, inner satellite of Haumea was discovered on June 30, 2005, formally termed S/2005 (2003 EL61) 2, and nicknamed "Blitzen". On September 7, 2006, both satellites were numbered and admitted into the official minor planet catalogue as (136108) 2003 EL61 I and II, respectively.
The permanent names of these moons were announced, together with that of 2003 EL61, by the International Astronomical Union on September 17, 2008: (136108) Haumea I Hiʻiaka and (136108) Haumea II Namaka. Each moon was named after a daughter of Haumea, the Hawaiian goddess of fertility and childbirth. Hiʻiaka is the goddess of dance and patroness of the Big Island of Hawaii, where the Mauna Kea Observatory is located. Nāmaka is the goddess of water and the sea; she cooled her sister Pele's lava as it flowed into the sea, turning it into new land.
In her legend, Haumea's many children came from different parts of her body. The dwarf planet Haumea appears to be almost entirely made of rock, with only a superficial layer of ice; most of the original icy mantle is thought to have been blasted off by the impact that spun Haumea into its current high speed of rotation, where the material formed into the small Kuiper belt objects in Haumea's collisional family. There could therefore be additional outer moons, smaller than Namaka, that have not yet been detected. However, HST observations have confirmed that no other moons brighter than 0.25% of the brightness of Haumea exist within the closest tenth of the distance (0.1% of the volume) where they could be held by Haumea's gravitational influence (its Hill sphere). This makes it unlikely that any more exist.
Hiʻiaka is the outer and, at roughly 350 km in diameter, the larger and brighter of the two moons. Strong absorption features observed at 1.5, 1.65 and 2 µm in its infrared spectrum are consistent with nearly pure crystalline water ice covering much of its surface. The unusual spectrum, and its similarity to absorption lines in the spectrum of Haumea, led Brown and colleagues to conclude that it was unlikely that the system of moons was formed by the gravitational capture of passing Kuiper belt objects into orbit around the dwarf planet: instead, the Haumean moons must be fragments of Haumea itself.
The sizes of both moons are calculated with the assumption that they have the same infrared albedo as Haumea, which is reasonable as their spectra show them to have the same surface composition. Haumea's albedo has been measured by the Spitzer Space Telescope: from ground-based telescopes, the moons are too small and close to Haumea to be seen independently. Based on this common albedo, the inner moon, Namaka, which is a tenth the mass of Hiʻiaka, would be about 170 km in diameter.
The Hubble Space Telescope (HST) has adequate angular resolution to separate the light from the moons from that of Haumea. Photometry of the Haumea triple system with HST's NICMOS camera has confirmed that the spectral line at 1.6 µm that indicates the presence of water ice is at least as strong in the moons' spectra as in Haumea's spectrum.
The moons of Haumea are too faint to detect with telescopes smaller than about 2 metres in aperture, though Haumea itself has a visual magnitude of 17.5, making it the third-brightest object in the Kuiper belt after Pluto and Makemake, and easily observable with a large amateur telescope.
Hiʻiaka orbits Haumea nearly circularly every 49 days. 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. Because the impact that created the moons of Haumea is thought to have occurred in the early history of the Solar System, over the following billions of years it should have been tidally damped into a more circular orbit. Namaka's orbit has likely been disturbed by orbital resonances with the more-massive Hiʻiaka due to converging orbits as they moved outward from Haumea due to tidal dissipation. They may have been caught in and then escaped from orbital resonance several times; they currently are in or at least close to an 8:3 resonance. This resonance strongly perturbs Namaka's orbit, which has a current precession of its argument of periapsis by about −6.5° per year, a precession period of 55 years.
At present, the orbits of the Haumean moons appear almost exactly edge-on from Earth, with Namaka having periodically occulted Haumea from 2009 to 2011. Observation of such transits would provide precise information on the size and shape of Haumea and its moons, as happened in the late 1980s with Pluto and Charon. The tiny change in brightness of the system during these occultations required at least a medium-aperture professional telescope for detection. Hiʻiaka last occulted Haumea in 1999, a few years before its discovery, and will not do so again for some 130 years. However, in a situation unique among regular satellites, the great torquing of Namaka's orbit by Hiʻiaka preserved the viewing angle of Namaka–Haumea transits for several more years.
|Eccentricity||Inclination (°)||Discovery date|
|1||Haumea II||Namaka||/nɑːˈmɑːkə/||≈ 170?||1.79±1.48
(≈ 0.05% Haumea)
|25657±91||18.2783±0.0076[note 3]||0.249±0.015[note 4]||113.013±0.075
(13.41±0.08 from Hiʻiaka)[note 4]
|2||Haumea I||Hiʻiaka||/hiːʔiːˈɑːkə/||≈ 310||17.9±1.1
(≈ 0.5% Haumea)
|49880±198||49.462±0.083[note 3]||0.0513±0.0078||126.356±0.064||January 2005|
|Discovered by||Michael E. Brown,
David Rabinowitz, et al.
|Discovery date||30 June 2005|
|MPC designation||Haumea II Namaka|
|(136108) 2003 EL61 II,
S/2005 (2003 EL61) 2
|Epoch JD 2454615.0|
|Eccentricity||0.249±0.015 (in 2009; variable)|
13.41°±0.08° relative to Hiʻiaka (in 2008; variable)
|~85 km (if albedo is same as primary's 0.7±0.1)|
|Mass||1.79 ± 1.48×1018 kg
(0.05% the mass of Haumea)
|(assumed to be near 1 g/cm3)|
|21.9 (4.6 difference from primary's 17.3)|
Namaka is only 1.5% as bright as its parent dwarf planet Haumea and is about 0.05% its mass. If it turns out to have a similar albedo, it would be about 170 km in diameter. Photometric observations indicate that its surface is made of water ice. Mutual events between 2009 and 2011 were expected to improve the knowledge of the orbits and masses of the components of the Haumean system, but interpreting those observations was greatly complicated by the unexpected non-tidally locked spin state of Hiʻiaka. Further observations of Hiʻiaka might allow to determine its rotation period and spin state more precisely, at which point it should be possible to remove its effect from the data obtained in 2009.
Hiʻiaka is above Haumea (center) in this Keck telescope image.
|Discovered by||Michael E. Brown,
David Rabinowitz, et al.
|Discovery date||26 January 2005|
|MPC designation||Haumea I Hiʻiaka|
|(136108) 2003 EL61 I,
S/2005 (2003 EL61) 1
|Mass||(1.79±0.11)×1019 kg (0.45% of Haumea)|
|20.3 (3.0 difference from primary's 17.3)|
Hiʻiaka was the first satellite discovered around Haumea. It is named after one of the daughters of Haumea, Hiʻiaka, the patron goddess of the Big Island of Hawaii, though at first it had gone by the nickname "Rudolph" by its discovery team. It orbits once every 49.12±0.03 d at a distance of 49880±198 km, with an eccentricity of 0.0513±0.0078 and an inclination of 126.356±0.064°.
Its measured brightness is 5.9±0.5%, translating into a diameter of about 22% of its primary, or in the range of 320 km, assuming similar albedo. To put this in perspective, this would make it larger than all but four of the asteroids, after 1 Ceres, 2 Pallas, 4 Vesta, and 10 Hygiea. In spite of its relatively large size, however, lightcurve studies suggest that Hi'iaka is not a gravitationally collapsed spheroid; they further suggest that Hi'iaka is not tidally locked and has a rotation period of about 9.8 hours.
The near infrared spectrum of Hiʻiaka is dominated by water-ice absorption bands, which means that its surface is made mainly of water ice. The presence of the band centered at 1.65 μm indicates that the surface water ice is primarily in the crystalline form. Currently it is unclear why water ice on the surface has not turned into amorphous form as would be expected due to its constant irradiation by cosmic rays.