Haumea

Haumea  (mostly astrological)

Low-resolution Hubble Space Telescope image of Haumea and its two moons, Hiʻiaka (top) and Namaka (bottom), June 2015

Discovery
Discovered by|

* Brown et al.
* Ortiz et al.

Discovery date|

* 7 March 2003 (Ortiz)
* 28 December 2004 (Brown)

Designations

MPC designation

| (136108) Haumea
Pronunciation| /haʊˈmeɪ.ə, ˌhɑːuː-/[nb 1]
Named after| Haumea

Alternative designations

| 2003 EL61 (provisional designation)
Minor planet category|

* Dwarf planet
* TNO[1][2]
* Haumea family
* trinary[3]

Adjectives| Haumean[7]
Orbital characteristics[10]
Epoch 17 December 2020 (JD 2459200.5)
Uncertainty parameter 2
Observation arc| 65 years and 291 days (24033 days)
Earliest precovery date| 22 March 1955
|{{{apsis}}}|helion}}| 51.585 astronomical unit|AU (7.7170 Tm)
|{{{apsis}}}|helion}}| 34.647 AU (5.1831 Tm)

Semi-major axis

| 43.116 AU (6.4501 Tm)
Eccentricity| 0.19642
Orbital period| 283.12 yr (103,410 days)[8]
Average Orbital speed| 4.53 km/s[nb 2]
Mean anomaly| 218.205°
Mean motion| 0° 0m 12.533s / day
Inclination| 28.2137°
Longitude of ascending node| 122.167°
|{{{apsis}}}|helion}}| ≈ 1 June 2133[9]
±2 days

|{{{apsis}}}|helion}}

| 239.041°
Known satellites| 2 (Hiʻiaka and Namaka)
Physical characteristics
Dimensions|

* ≈ 2,100 × 1,680 × 1,074 km[nb 3][11]
* 2,322±60 × 1,704±8 × 1,026±32 km[nb 4][12]

Mean radius|

* ≈ 780 km[nb 3]
* 798±6 km to 816 km[nb 5]

Surface area| ≈ 8.14×106 km2[nb 3][13]
Volume| ≈ 1.98×109 km3[nb 3][14]
0.0018 Earths
Mass| 3.95244+0.01109
−0.01103×1021 kg[15]
0.00066 Earths
Mean density|

* ≈ 2.018 g/cm3[nb 3]
* 1.885±0.080 g/cm3 to 1.757 g/cm3[nb 5]

Equatorial surface gravity

| 0.93 m/s2 at poles
to 0.24 m/s2 at longest axis

Equatorial escape velocity

| 1 km/s at poles
to 0.71 km/s at longest axis
Sidereal rotation period| 3.915341±0.000005 h[16]
(0.163139208 d)
Axial tilt| ≈ 126° (to orbit; assumed)
81.2° or 78.9° (to ecliptic)[nb 6]
North pole right ascension| 282.6°±1.2°[17]: 3174
North pole declination| −13.0°±1.3° or −11.8°±1.2°[17]: 3174
Geometric albedo|

* ≈ 0.66 geometric[nb 3]
* ≤ 0.51±0.02 geometric[12]
* 0.33±0.03 Bond[19]

Physics| < 50 K[20]

Spectral type

* BB (neutral)
* B−V = 0.64, V−R = 0.33[21]
* B0−V0 = 0.646[22]

Apparent magnitude| 17.3 (opposition)[23][24]
Absolute magnitude (H)| 0.428±0.011 (V-band)[16] * 0.2[8]

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. From that announcement, it received the provisional designation 2003 EL61.

On 17 September 2008, it was named after Haumea, the Hawaiian goddess of childbirth and fertility, under the expectation by the International Astronomical Union (IAU) that it would prove to be a dwarf planet. Nominal estimates make it the third-largest known trans-Neptunian object, after Eris and Pluto, and approximately the size of Uranus's moon Titania. Precovery images of Haumea have been identified back to 22 March 1955.[8]

Haumea's mass is about one-third that of Pluto and 1/1400 that of Earth. Although its shape has not been directly observed, calculations from its light curve are consistent with it being a Jacobi ellipsoid (the shape it would be if it were a dwarf planet), with its major axis twice as long as its minor. In October 2017, astronomers announced the discovery of a ring system around Haumea, representing the first ring system discovered for a trans-Neptunian object and a dwarf planet.

Haumea's gravity was until recently thought to be sufficient for it to have relaxed into hydrostatic equilibrium, though that is now unclear. Haumea's elongated shape, together with its rapid rotation, rings, and high albedo (from a surface of crystalline water ice), is thought to be the consequences of a giant collision, which left Haumea the largest member of a collisional family (the Haumea family) that includes several large trans-Neptunian objects and Haumea's two known moons, Hiʻiaka and Namaka.

## Contents

* 1 History
* 1.1 Discovery
* 1.2 Name and symbol
* 2 Orbit
* 2.1 Possible resonance with Neptune
* 3 Rotation
* 4 Physical characteristics
* 4.1 Size, shape, and composition
* 4.2 Surface
* 5 Ring
* 6 Satellites
* 7 Collisional family
* 8 Exploration
* 9 See also
* 10 Notes
* 11 References
* 12 External links

## History

### Discovery

Main article: Astronomy:Controversy over the discovery of Haumea

Two teams claim credit for the discovery of Haumea. A team consisting of Mike Brown of Caltech, David Rabinowitz of Yale University, and Chad Trujillo of Gemini Observatory in Hawaii discovered Haumea on 28 December 2004, on images they had taken on 6 May 2004. On 20 July 2005, they published an online abstract of a report intended to announce the discovery at a conference in September 2005.[26]

At around this time, José Luis Ortiz Moreno and his team at the Instituto de Astrofísica de Andalucía at Sierra Nevada Observatory in Spain found Haumea on images taken on 7–10 March 2003.[27] Ortiz emailed the Minor Planet Center with their discovery on the night of 27 July 2005.[27]

Brown initially conceded discovery credit to Ortiz,[28] but came to suspect the Spanish team of fraud upon learning that the Spanish observatory had accessed Brown's observation logs the day before the discovery announcement, a fact that they did not disclose in the announcement as would be customary. Those logs included enough information to allow the Ortiz team to precover Haumea in their 2003 images, and they were accessed again just before Ortiz scheduled telescope time to obtain confirmation images for a second announcement to the MPC on 29 July. Ortiz later admitted he had accessed the Caltech observation logs but denied any wrongdoing, stating he was merely verifying whether they had discovered a new object.[29]

IAU protocol is that discovery credit for a minor planet goes to whoever first submits a report to the MPC (Minor Planet Center) with enough positional data for a decent determination of its orbit, and that the credited discoverer has priority in choosing a name. However, the IAU announcement on 17 September 2008, that Haumea had been named by a dual committee established for bodies expected to be dwarf planets, did not mention a discoverer. The location of discovery was listed as the Sierra Nevada Observatory of the Spanish team,[30][31] but the chosen name, Haumea, was the Caltech proposal. Ortiz's team had proposed "Ataecina", the ancient Iberian goddess of spring;[27] as a chthonic deity, it would have been appropriate for a plutino, which Haumea was not.

### Name and symbol

Until it was given a permanent name, the Caltech discovery team used the nickname "Santa" among themselves, because they had discovered Haumea on 28 December 2004, just after Christmas.[32] The Spanish team were the first to file a claim for discovery to the Minor Planet Center, in July 2005. On 29 July 2005, Haumea was given the provisional designation 2003 EL61, based on the date of the Spanish discovery image. On 7 September 2006, it was numbered and admitted into the official minor planet catalog as (136108) 2003 EL61.

Following guidelines established at the time by the IAU that classical Kuiper belt objects be given names of mythological beings associated with creation,[33] in September 2006 the Caltech team submitted formal names from Hawaiian mythology to the IAU for both (136108) 2003 EL61 and its moons, in order "to pay homage to the place where the satellites were discovered".[34] The names were proposed by David Rabinowitz of the Caltech team.[25] Haumea is the matron goddess of the island of Hawaiʻi, where Gemini and W. M. Keck Observatory are located on Mauna Kea. In addition, she is identified with Papa, the goddess of the earth and wife of Wākea (space),[35] which, at the time, seemed appropriate because Haumea was thought to be composed almost entirely of solid rock, without the thick ice mantle over a small rocky core typical of other known Kuiper belt objects.[36][37] Lastly, Haumea is the goddess of fertility and childbirth, with many children who sprang from different parts of her body;[35] this corresponds to the swarm of icy bodies thought to have broken off the main body during an ancient collision.[37] The two known moons, also believed to have formed in this manner,[37] are thus named after two of Haumea's daughters, Hiʻiaka and Nāmaka.[36]

The proposal by the Ortiz team, Ataecina, did not meet IAU naming requirements, because the names of chthonic deities were reserved for stably resonant trans-Neptunian objects such as plutinos that resonate 3:2 with Neptune, whereas Haumea was in an intermittent 7:12 resonance and so by some definitions was not a resonant body. The naming criteria would be clarified in late 2019, when the IAU decided that chthonic figures were to be used specifically for plutinos.

A planetary symbol for Haumea, ⟨⟩, is included in Unicode at U+1F77B.[38] Planetary symbols are no longer much used in astronomy, and 🝻 is mostly used by astrologers,[39] but has also been used by NASA.[40] The symbol was designed by Denis Moskowitz, a software engineer in Massachusetts; it combines and simplifies Hawaiian petroglyphs meaning 'woman' and 'childbirth'.[41]

## Orbit

Haumea's orbit outside of Neptune is similar to Makemake's. The positions are as of January 1, 2018.

Haumea has an orbital period of 284 Earth years, a perihelion of 35 AU, and an orbital inclination of 28°.[8] It passed aphelion in early 1992, and is currently more than 50 AU from the Sun.[23] It will come to perihelion in 2133.[9] Haumea's orbit has a slightly greater eccentricity than that of the other members of its collisional family. This is thought to be due to Haumea's weak 7:12 orbital resonance with Neptune gradually modifying its initial orbit over the course of a billion years,[37][42] through the Kozai effect, which allows the exchange of an orbit's inclination for increased eccentricity.[37][43][44]

With a visual magnitude of 17.3,[23] Haumea is the third-brightest object in the Kuiper belt after Pluto and Makemake, and easily observable with a large amateur telescope.[45] However, because the planets and most small Solar System bodies share a common orbital alignment from their formation in the primordial disk of the Solar System, most early surveys for distant objects focused on the projection on the sky of this common plane, called the ecliptic.[46] As the region of sky close to the ecliptic became well explored, later sky surveys began looking for objects that had been dynamically excited into orbits with higher inclinations, as well as more distant objects, with slower mean motions across the sky.[47][48] These surveys eventually covered the location of Haumea, with its high orbital inclination and current position far from the ecliptic.

Haumea's future orbit is unlikely to be stable over the course of the Solar System. A study which simulated the future orbits of 34 trans-Neptunian objects showed Haumea was the most statistically likely to be ejected out of its orbit into outer space or the inner Solar System over the next billion years.[49]

### Possible resonance with Neptune

The libration of Haumea's nominal orbit in a rotating frame, with Neptune stationary (see 2 Pallas for an example of non-librating)

The libration angle ϕ of Haumea's weak 7:12 resonance with Neptune, ϕ=12λ−7λN−5ϖ−1Ω, over the next 5 million years

Haumea is thought to be in an intermittent 7:12 orbital resonance with Neptune.[37] Its ascending node Ω precesses with a period of about 4.6 million years, and the resonance is broken twice per precession cycle, or every 2.3 million years, only to return a hundred thousand years or so later.[2] As this is not a stable resonance, Marc Buie qualifies it as non-resonant.[50]

## Rotation

Haumea displays large fluctuations in brightness over a period of 3.9 hours, which can only be explained by a rotational period of this length.[51] This is faster than any other known equilibrium body in the Solar System, and indeed faster than any other known body larger than 100 km in diameter.[45] While most rotating bodies in equilibrium are flattened into oblate spheroids, Haumea rotates so quickly that it is distorted into a triaxial ellipsoid. If Haumea were to rotate much more rapidly, it would distort itself into a dumbbell shape and split in two.[25] This rapid rotation is thought to have been caused by the impact that created its satellites and collisional family.[37]

The plane of Haumea's equator is oriented nearly edge-on from Earth at present and is also slightly offset to the orbital planes of its ring and its outermost moon Hiʻiaka. Although initially assumed to be coplanar to Hiʻiaka's orbital plane by Ragozzine and Brown in 2009, their models of the collisional formation of Haumea's satellites consistently suggested Haumea's equatorial plane to be at least aligned with Hiʻiaka's orbital plane by approximately 1°.[52] This was supported with observations of a stellar occultation by Haumea in 2017, which revealed the presence of a ring approximately coincident with the plane of Hiʻiaka's orbit and Haumea's equator.[12] A mathematical analysis of the occultation data by Kondratyev and Kornoukhov in 2018 placed constraints on the relative inclination angles of Haumea's equator to the orbital planes of its ring and Hiʻiaka, which were found to be inclined 3.2°±1.4° and 2.0°±1.0° relative to Haumea's equator, respectively.[17]

## Physical characteristics

### Size, shape, and composition

The size of a Solar System object can be deduced from its optical magnitude, its distance, and its albedo. Objects appear bright to Earth observers either because they are large or because they are highly reflective. If their reflectivity (albedo) can be ascertained, then a rough estimate can be made of their size. For most distant objects, the albedo is unknown, but Haumea is large and bright enough for its thermal emission to be measured, which has given an approximate value for its albedo and thus its size.[53] However, the calculation of its dimensions is complicated by its rapid rotation. The rotational physics of deformable bodies predicts that over as little as a hundred days,[45] a body rotating as rapidly as Haumea will have been distorted into the equilibrium form of a triaxial ellipsoid. It is thought that most of the fluctuation in Haumea's brightness is caused not by local differences in albedo but by the alternation of the side view and ends view as seen from Earth.[45]

The rotation and amplitude of Haumea's light curve were argued to place strong constraints on its composition. If Haumea were in hydrostatic equilibrium and had a low density like Pluto, with a thick mantle of ice over a small rocky core, its rapid rotation would have elongated it to a greater extent than the fluctuations in its brightness allow. Such considerations constrained its density to a range of 2.6–3.3 g/cm3.[54][45] By comparison, the Moon, which is rocky, has a density of 3.3 g/cm3, whereas Pluto, which is typical of icy objects in the Kuiper belt, has a density of 1.86 g/cm3. Haumea's possible high density covered the values for silicate minerals such as olivine and pyroxene, which make up many of the rocky objects in the Solar System. This also suggested that the bulk of Haumea was rock covered with a relatively thin layer of ice. A thick ice mantle more typical of Kuiper belt objects may have been blasted off during the impact that formed the Haumean collisional family.[37]

Because Haumea has moons, the mass of the system can be calculated from their orbits using Kepler's third law. The result is 4.2×1021 kg, 28% the mass of the Plutonian system and 6% that of the Moon. Nearly all of this mass is in Haumea.[52][55] Several ellipsoid-model calculations of Haumea's dimensions have been made. The first model produced after Haumea's discovery was calculated from ground-based observations of Haumea's light curve at optical wavelengths: it provided a total length of 1,960 to 2,500 km and a visual albedo (pv) greater than 0.6.[45] The most likely shape is a triaxial ellipsoid with approximate dimensions of 2,000 × 1,500 × 1,000 km, with an albedo of 0.71.[45] Observations by the Spitzer Space Telescope gave a diameter of 1,150+250
−100 km and an albedo of 0.84+0.1
−0.2, from photometry at infrared wavelengths of 70 μm.[53] Subsequent light-curve analyses have suggested an equivalent circular diameter of 1,450 km.[56] In 2010 an analysis of measurements taken by Herschel Space Telescope together with the older Spitzer Telescope measurements yielded a new estimate of the equivalent diameter of Haumea—about 1300 km.[57] These independent size estimates overlap at an average geometric mean diameter of roughly 1,400 km. In 2013 the Herschel Space Telescope measured Haumea's equivalent circular diameter to be roughly 1,240+69
−58 km.[58]

The calculated ellipsoid shape of Haumea, 1,960×1,518×996 km (assuming an albedo of 0.73). At the left are the minimum and maximum equatorial silhouettes (1,960×996 and 1,518×996 km); at the right is the view from the pole (1,960×1,518 km).

Haumea's rapid rotation (of just under 4 hours) elongated it into a triaxial ellipsoid shape. Haumea exhibits distinguishable variations in colour as it rotates, indicative of a dark red spot on its surface as depicted here.

However the observations of a stellar occultation in January 2017 cast a doubt on all those conclusions. The measured shape of Haumea, while elongated as presumed before, appeared to have significantly larger dimensions - according to the data obtained from the occultation Haumea is approximately the diameter of Pluto along its longest axis and about half that at its poles.[12] The resulting density calculated from the observed shape of Haumea was about 1.8 g/cm3 - more in line with densities of other large TNOs. This resulting shape appeared to be inconsistent with a homogenous body in hydrostatic equilibrium,[12] though Haumea appears to be one of the largest trans-Neptunian objects discovered nonetheless,[53] smaller than Eris, Pluto, similar to Makemake, and possibly Gonggong, and larger than Sedna, Quaoar, and Orcus.

A 2019 study attempted to resolve the conflicting measurements of Haumea's shape and density using numerical modeling of Haumea as a differentiated body. It found that dimensions of ≈ 2,100 × 1,680 × 1,074 km (modeling the long axis at intervals of 25 km) were a best-fit match to the observed shape of Haumea during the 2017 occultation, while also being consistent with both surface and core scalene ellipsoid shapes in hydrostatic equilibrium.[11] The revised solution for Haumea's shape implies that it has a core of approximately 1,626 × 1,446 × 940 km, with a relatively high density of ≈ 2.68 g/cm3, indicative of a composition largely of hydrated silicates such as kaolinite. The core is surrounded by an icy mantle that ranges in thickness from about 70 km at the poles to 170 km along its longest axis, comprising up to 17% of Haumea's mass. Haumea's mean density is estimated at ≈ 2.018 g/cm3, with an albedo of ≈ 0.66.[11]

### Surface

In 2005, the Gemini and Keck telescopes obtained spectra of Haumea which showed strong crystalline water ice features similar to the surface of Pluto's moon Charon.[20] This is peculiar, because crystalline ice forms at temperatures above 110 K, whereas Haumea's surface temperature is below 50 K, a temperature at which amorphous ice is formed.[20] In addition, the structure of crystalline ice is unstable under the constant rain of cosmic rays and energetic particles from the Sun that strike trans-Neptunian objects.[20] The timescale for the crystalline ice to revert to amorphous ice under this bombardment is on the order of ten million years,[59] yet trans-Neptunian objects have been in their present cold-temperature locations for timescales of billions of years.[42]

Radiation damage should also redden and darken the surface of trans-Neptunian objects where the common surface materials of organic ices and tholin-like compounds are present, as is the case with Pluto. Therefore, the spectra and colour suggest Haumea and its family members have undergone recent resurfacing that produced fresh ice. However, no plausible resurfacing mechanism has been suggested.[22]

Haumea is as bright as snow, with an albedo in the range of 0.6–0.8, consistent with crystalline ice.[45] Other large TNOs such as Eris appear to have albedos as high or higher.[60] Best-fit modeling of the surface spectra suggested that 66% to 80% of the Haumean surface appears to be pure crystalline water ice, with one contributor to the high albedo possibly hydrogen cyanide or phyllosilicate clays.[20] Inorganic cyanide salts such as copper potassium cyanide may also be present.[20]

However, further studies of the visible and near infrared spectra suggest a homogeneous surface covered by an intimate 1:1 mixture of amorphous and crystalline ice, together with no more than 8% organics. The absence of ammonia hydrate excludes cryovolcanism and the observations confirm that the collisional event must have happened more than 100 million years ago, in agreement with the dynamic studies.[61] The absence of measurable methane in the spectra of Haumea is consistent with a warm collisional history that would have removed such volatiles,[20] in contrast to Makemake.[62]

In addition to the large fluctuations in Haumea's light curve due to the body's shape, which affect all colours equally, smaller independent colour variations seen in both visible and near-infrared wavelengths show a region on the surface that differs both in colour and in albedo.[63][64] More specifically, a large dark red area on Haumea's bright white surface was seen in September 2009, possibly an impact feature, which indicates an area rich in minerals and organic (carbon-rich) compounds, or possibly a higher proportion of crystalline ice.[51][65] Thus Haumea may have a mottled surface reminiscent of Pluto, if not as extreme.

## Ring

Haumea's 3.9155-hour rotation within its discovered ring

A stellar occultation, observed on 21 January 2017 and described in an October 2017 Nature article, indicated the presence of a ring around Haumea. This represents the first ring system discovered for a TNO.[12][66] The ring has a radius of about 2,287 km, a width of ~70 km and an opacity of 0.5. It is well within Haumea's Roche limit, which would be at a radius of about 4,400 km if it were spherical (being nonspherical pushes the limit out farther).[12]

The ring plane is inclined 3.2°±1.4° with respect to Haumea's equatorial plane and approximately coincides with the orbital plane of its larger, outer moon Hiʻiaka.[12][67] The ring is also close to the 1:3 orbit-spin resonance with Haumea's rotation (which is at a radius of 2,285 ± 8 km from Haumea's center). The ring is estimated to contribute 5% to the total brightness of Haumea.[12]

In a study about the dynamics of ring particles published in 2019, Othon Cabo Winter and colleagues have shown that the 1:3 resonance with Haumea's rotation is dynamically unstable, but that there is a stable region in the phase space consistent with the location of Haumea's ring. This indicates that the ring particles originate on circular, periodic orbits that are close to, but not inside, the resonance.[68]

## Satellites

| Parts of this astronomy (those related to section) need to be updated. The reason given is: The orbits, sizes, masses, and formation hypothesis of Namaka and Hi'iaka have been revised in newer studies by Proudfoot et al. (2024), Vara Lubiano (2023), and Noviello et al. (2022). Please update this astronomy to reflect recent events or newly available information. (July 2025)

|

Main article: Astronomy:Moons of Haumea

Haumea and its orbiting moons, imaged by Hubble in 2008. Hiʻiaka is the brighter, outermost moon, while Namaka is the fainter, inner moon.

Two small satellites have been discovered orbiting Haumea, (136108) Haumea I, named Hiʻiaka, and (136108) Haumea II, named Namaka.[30] Darin Ragozzine and Michael Brown discovered both in 2005, through observations of Haumea using the W. M. Keck Observatory.

Hiʻiaka, at first nicknamed "Rudolph" by the Caltech team,[69] was discovered 26 January 2005.[55] It is the outer and, at roughly 310 km in diameter, the larger and brighter of the two, and orbits Haumea in a nearly circular path every 49 days.[70] Strong absorption features at 1.5 and 2 micrometres in the infrared spectrum are consistent with nearly pure crystalline water ice covering much of the surface.[71] The unusual spectrum, along with similar absorption lines on Haumea, led Brown and colleagues to conclude that capture was an unlikely model for the system's formation, and that the Haumean moons must be fragments of Haumea itself.[42]

Namaka, the smaller, inner satellite of Haumea, was discovered on 30 June 2005,[72] and nicknamed "Blitzen". It is a tenth the mass of Hiʻiaka, orbits Haumea in 18 days in a highly elliptical, non-Keplerian orbit, and as of 2008[update] is inclined 13° from the larger moon, which perturbs its orbit.[73] The relatively large eccentricities together with the mutual inclination of the orbits of the satellites are unexpected as they should have been damped by the tidal effects. A relatively recent passage by a 3:1 resonance with Hiʻiaka might explain the current excited orbits of the Haumean moons.[52]

From around 2008 to 2011,[74] the orbits of the Haumean moons appeared almost exactly edge-on from Earth, with Namaka periodically occulting Haumea.[75] Observation of such transits would have provided precise information on the size and shape of Haumea and its moons,[76] as happened in the late 1980s with Pluto and Charon.[77] The tiny change in brightness of the system during these occultations would have required at least a medium-aperture professional telescope for detection.[76][78] Hiʻiaka last occulted Haumea in 1999, a few years before discovery, and will not do so again for some 130 years.[79] However, in a situation unique among regular satellites, Namaka's orbit was being greatly torqued by Hiʻiaka, which preserved the viewing angle of Namaka–Haumea transits for several more years.[73][76][78] One occultation event was observed on 19 June 2009, from the Pico dos Dias Observatory in Brazil.[80]

Haumean system  Name  | Diameter (km)[81][82][83] | Semi-major axis (km)[84] | Mass (kg)[84] | Discovery date[85]

|
|
|
|

Haumea  | 2 322 × 1,704 × 1,026  |  | (4.006 ± 0.040) × 1021 | 7 March 2003[85]
Hiʻiaka  | 370±20 | 49 880  | (1.79 ± 0.11) x 1019 | 26 January 2005
Namaka  | 150±50 | 25 657  | (1.79 ± 1.48) x 1018 | 2005

## Collisional family

A chart showing confirmed[86][87] Haumea family members to scale (as of 2025[update]). Unmeasured members are shown with estimated diameters using an assumed albedo of 0.7.

Haumea is the largest member of its collisional family, a group of astronomical objects with similar physical and orbital characteristics thought to have formed when a larger progenitor was shattered by an impact.[37] This family is the first to be identified among TNOs and includes—beside Haumea and its moons—(55636) 2002 TX300 (≈364 km), (24835) 1995 SM55 (≈174 km), (19308) 1996 TO66 (≈200 km), (120178) 2003 OP32 (≈230 km), and (145453) 2005 RR43 (≈252 km).[3] Brown and colleagues proposed that the family were a direct product of the impact that removed Haumea's ice mantle,[37] but a second proposal suggests a more complicated origin: that the material ejected in the initial collision instead coalesced into a large moon of Haumea, which was later shattered in a second collision, dispersing its shards outwards.[88] This second scenario appears to produce a dispersion of velocities for the fragments that is more closely matched to the measured velocity dispersion of the family members.[88]

The presence of the collisional family could imply that Haumea and its "offspring" might have originated in the scattered disc. In today's sparsely populated Kuiper belt, the chance of such a collision occurring over the age of the Solar System is less than 0.1 percent.[89] The family could not have formed in the denser primordial Kuiper belt because such a close-knit group would have been disrupted by Neptune's migration into the belt—the believed cause of the belt's current low density.[89] Therefore, it appears likely that the dynamic scattered disc region, in which the possibility of such a collision is far higher, is the place of origin for the object that generated Haumea and its kin.[89]

Because it would have taken at least a billion years for the group to have diffused as far as it has, the collision which created the Haumea family is believed to have occurred at least that long ago.[3]

## Exploration

Haumea imaged by the New Horizons spacecraft on 6 October 2007

Haumea was observed from afar by the New Horizons spacecraft in October 2007, January 2017, and May 2020, from distances of 49 AU, 59 AU, and 63 AU, respectively.[19] The spacecraft's outbound trajectory permitted observations of Haumea at high phase angles that are otherwise unobtainable from Earth, enabling the determination of the light scattering properties and phase curve behavior of Haumea's surface.[19]

A flyby mission could reach Haumea in 16.45 years if was launched on 1 November 2026, 23 September 2037, and 29 October 2038.[90] Haumea could become a target for an exploration mission,[91] and an example of this work is a preliminary study on a probe to Haumea and its moons (at 35–51 AU).[92] Probe mass, power source, and propulsion systems are key technology areas for this type of mission.[91]

## See also

* 20000 Varuna – a large, rapidly-rotating trans-Neptunian object with an elongated ellipsoid shape
* 208996 Achlys – another large, rapidly-rotating trans-Neptunian object with an elongated ellipsoid shape similar to Haumea
* Astronomical naming conventions
* How I Killed Pluto and Why It Had It Coming – A 2010 memoir by Mike Brown
* List of Solar System objects by size

## Notes

1. ↑ how-MAY-ə, with three syllables according to the English pronunciation in Hawaii,[4] or HAH-oo-MAY-ə with four syllables according to Brown's students.[5][6]
2. ↑ Assuming a circular orbit with negligible eccentricity, the mean orbital speed can be approximated by the time T it takes to complete one revolution around its orbital circumference, with the radius being its semi-major axis a:  v≈2πaT.
3. ↑ 3.0 3.1 3.2 3.3 3.4 3.5 Best fit physical model assuming hydrostatic equilibrium for Haumea.[11]
4. ↑ Occultation-derived model based on the assumption Haumea's ring does not contribute to its total brightness.[12]
5. ↑ 5.0 5.1 Occultation-derived model based on the upper-limit assumption that Haumea's ring contributes 5% to its total brightness.[12]
6. ↑ Kondratyev and Kornoukhov (2018) give Haumea's north pole orientation in terms of equatorial coordinates, where α is right ascension and δ is declination.[17]: 3174 Transforming equatorial coordinates to ecliptic coordinates gives λ ≈ 282.5° and β ≈ 9.9° for the first solution of (α, δ) = (282.6°, –13.0°), or λ ≈ 282.6° and β ≈ 11.1° for the second solution of (α, δ) = (282.6°, –11.8°).[18] The ecliptic latitude, β, is the angular offset from the ecliptic plane, whereas inclination i with respect to the ecliptic is the angular offset from the ecliptic north pole at  β = +90° ; i with respect to the ecliptic would be the complement of β, which is expressed by the difference  i = 90° – β. Thus, Haumea's axial tilt is 81.2° or 78.9° with respect to the ecliptic, for the first and second β values, respectively.

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3. ↑ 3.0 3.1 3.2 Ragozzine, D.; Brown, M. E. (2007). "Candidate Members and Age Estimate of the Family of Kuiper Belt Object 2003 EL61". Astronomical Journal 134 (6): 2160–2167. doi:10.1086/522334. Bibcode: 2007AJ....134.2160R.
4. ↑ New dwarf planet named for Hawaiian goddess (HeraldNet, 19 September 2008)
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6. ↑ "365 Days of Astronomy". 31 March 2009. http://365daysofastronomy.org/2009/03/31/march-31st/.
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8. ↑ 8.0 8.1 8.2 8.3 "Jet Propulsion Laboratory Small-Body Database Browser: 136108 Haumea (2003 EL61)". NASA's Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2136108.
9. ↑ 9.0 9.1 "Horizons Batch for Haumea at perihelion around 1 June 2133". JPL Horizons. Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/horizons_batch.cgi?batch=1&COMMAND='20136108'&START_TIME='2133-05-25'&STOP_TIME='2133-06-14'&STEP_SIZE='3 hours'&QUANTITIES='19'.
10. ↑ "(136108) Haumea = 2003 EL61". Minor Planet Center. International Astronomical Union. https://www.minorplanetcenter.net/db_search/show_object?object_id=136108.
11. ↑ 11.0 11.1 11.2 11.3 Dunham, E. T.; Desch, S. J.; Probst, L. (April 2019). "Haumea's Shape, Composition, and Internal Structure". The Astrophysical Journal 877 (1): 11. doi:10.3847/1538-4357/ab13b3. Bibcode: 2019ApJ...877...41D.
12. ↑ 12.00 12.01 12.02 12.03 12.04 12.05 12.06 12.07 12.08 12.09 12.10 Ortiz, J. L.Expression error: Unrecognized word "etal". (2017). "The size, shape, density and ring of the dwarf planet Haumea from a stellar occultation". Nature 550 (7675): 219–223. doi:10.1038/nature24051. PMID 29022593. Bibcode: 2017Natur.550..219O. http://www.astrosurf.com/sogorb/occultations/nature24051.pdf. Retrieved 2020-08-19.
13. ↑ "Ellipsoid surface area: 8.13712×10^6 km2". 20 December 2019. https://www.wolframalpha.com/input/?i=ellipsoid+surface+area+semi-axis+lengths+1050+840+537.
14. ↑ "Ellipsoid volume: 1.98395×10^9 km3". 20 December 2019. https://www.wolframalpha.com/input/?i=ellipsoid+volume+semi-axis+lengths+1050+840+537.
15. ↑ Proudfoot, Benjamin C. N.; Ragozzine, Darin A.; Giforos, William; Grundy, Will M.; MacDonald, Mariah; Oldroyd, William J. (March 2024). "Beyond Point Masses. III. Detecting Haumea's Nonspherical Gravitational Field". The Planetary Science Journal 5 (3): 69. doi:10.3847/PSJ/ad26e9. Bibcode: 2024PSJ.....5...69P.
16. ↑ 16.0 16.1 Santos-Sanz, P.; Lellouch, E.; Groussin, O.; Lacerda, P.; Muller, T. G.; Ortiz, J. L.; Kiss, C.; Vilenius, E. et al. (August 2017). ""TNOs are Cool": A survey of the trans-Neptunian region XII. Thermal light curves of Haumea, 2003 VS2 and 2003 AZ84 with Herschel/PACS". Astronomy & Astrophysics 604 (A95): 19. doi:10.1051/0004-6361/201630354. Bibcode: 2017A&A...604A..95S.2003+VS2+and+2003+AZ84+with+Herschel/PACS&rft.jtitle=Astronomy+&+Astrophysics&rft.aulast=Santos-Sanz&rft.aufirst=P.&rft.au=Santos-Sanz, P.&rft.au=Lellouch, E.&rft.au=Groussin, O.&rft.au=Lacerda, P.&rft.au=Muller, T.+G.&rft.au=Ortiz, J.+L.&rft.au=Kiss, C.&rft.au=Vilenius, E.&rft.au=Stansberry, J.&rft.date=August+2017&rft.volume=604&rft.issue=A95&rft.pages=19&rft_id=info:doi/10.1051/0004-6361/201630354&rft_id=info:bibcode/2017A&A...604A..95S;&rfr_id=info:sid/en.wikibooks.org:Astronomy:Haumea">
17. ↑ 17.0 17.1 17.2 17.3 Kondratyev, B. P.; Kornoukhov, V. S. (August 2018). "Determination of the body of the dwarf planet Haumea from observations of a stellar occultation and photometry data". Monthly Notices of the Royal Astronomical Society 478 (3): 3159–3176. doi:10.1093/mnras/sty1321. Bibcode: 2018MNRAS.478.3159K.
18. ↑ "Coordinate Transformation & Galactic Extinction Calculator". NASA/IPAC Extragalactic Database. California Institute of Technology. https://ned.ipac.caltech.edu/forms/calculator.html. Equatorial → Ecliptic, J2000 for equinox and epoch. NOTE: When inputting equatorial coordinates, specify the units in the format "282.6d" instead of "282.6".
19. ↑ 19.0 19.1 19.2 Verbiscer, Anne J.Expression error: Unrecognized word "etal". (April 2022). "The Diverse Shapes of Dwarf Planet and Large KBO Phase Curves Observed from New Horizons". The Planetary Science Journal 3 (4): 31. doi:10.3847/PSJ/ac63a6. 95. Bibcode: 2022PSJ.....3...95V.
20. ↑ 20.0 20.1 20.2 20.3 20.4 20.5 20.6 Chadwick A. Trujillo; Michael E. Brown; Kristina Barkume; Emily Shaller; David L. Rabinowitz (2007). "The Surface of 2003 EL61 in the Near Infrared". Astrophysical Journal 655 (2): 1172–1178. doi:10.1086/509861. Bibcode: 2007ApJ...655.1172T.
21. ↑ Snodgrass, C.; Carry, B.; Dumas, C.; Hainaut, O. (February 2010). "Characterisation of candidate members of (136108) Haumea's family". Astronomy and Astrophysics 511: A72. doi:10.1051/0004-6361/200913031. Bibcode: 2010A&A...511A..72S.
22. ↑ 22.0 22.1 Rabinowitz, D. L.; Schaefer, Bradley E.; Schaefer, Martha; Tourtellotte, Suzanne W. (2008). "The Youthful Appearance of the 2003 EL61 Collisional Family". The Astronomical Journal 136 (4): 1502–1509. doi:10.1088/0004-6256/136/4/1502. Bibcode: 2008AJ....136.1502R.
23. ↑ 23.0 23.1 23.2 "AstDys (136108) Haumea Ephemerides". Department of Mathematics, University of Pisa, Italy. https://newton.spacedys.com/astdys/index.php?pc=1.1.3.0&n=Haumea.
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35. ↑ 35.0 35.1 Robert D. Craig (2004). Handbook of Polynesian Mythology. ABC-CLIO. p. 128. ISBN 978-1-57607-894-5. https://books.google.com/books?id=LOZuirJWXvUC&q=haumea&pg=PA128. Retrieved 2020-11-11.
36. ↑ 36.0 36.1 "News Release – IAU0807: IAU names fifth dwarf planet Haumea". International Astronomical Union. 2008-09-17. http://www.iau.org/public_press/news/release/iau0807/.
37. ↑ 37.00 37.01 37.02 37.03 37.04 37.05 37.06 37.07 37.08 37.09 Brown, M. E.; Barkume, K. M.; Ragozzine, D.; Schaller, L. (2007). "A collisional family of icy objects in the Kuiper belt". Nature 446 (7133): 294–296. doi:10.1038/nature05619. PMID 17361177. Bibcode: 2007Natur.446..294B. https://authors.library.caltech.edu/34346/2/nature05619-s1.pdf. Retrieved 2019-07-14.
38. ↑ "Proposed New Characters: The Pipeline". https://www.unicode.org/alloc/Pipeline.html.
39. ↑ Miller, Kirk (26 October 2021). "Unicode request for dwarf-planet symbols". https://www.unicode.org/L2/L2021/21224-dwarf-planet-syms.pdf.
40. ↑ JPL/NASA (22 April 2015). "What is a Dwarf Planet?". https://www.jpl.nasa.gov/infographics/what-is-a-dwarf-planet.
41. ↑ Anderson, Deborah (4 May 2022). "Out of this World: New Astronomy Symbols Approved for the Unicode Standard". The Unicode Consortium. http://blog.unicode.org/2022/05/out-of-this-world-new-astronomy-symbols.html.
42. ↑ 42.0 42.1 42.2 Michael E. Brown. "The largest Kuiper belt objects". Caltech. http://www.gps.caltech.edu/~mbrown/papers/ps/kbochap.pdf.
43. ↑ Nesvorný, D; Roig, F. (2001). "Mean Motion Resonances in the Transneptunian Region Part II: The 1 : 2, 3: 4, and Weaker Resonances". Icarus 150 (1): 104–123. doi:10.1006/icar.2000.6568. Bibcode: 2001Icar..150..104N.
44. ↑ Kuchner, Marc J.; Brown, Michael E.; Holman, Matthew (2002). "Long-Term Dynamics and the Orbital Inclinations of the Classical Kuiper Belt Objects". The Astronomical Journal 124 (2): 1221–1230. doi:10.1086/341643. Bibcode: 2002AJ....124.1221K.
45. ↑ 45.0 45.1 45.2 45.3 45.4 45.5 45.6 45.7 Rabinowitz, D. L.; Barkume, Kristina; Brown, Michael E.; Roe, Henry; Schwartz, Michael; Tourtellotte, Suzanne; Trujillo, Chad (2006). "Photometric Observations Constraining the Size, Shape, and Albedo of 2003 EL61, a Rapidly Rotating, Pluto-Sized Object in the Kuiper Belt". Astrophysical Journal 639 (2): 1238–1251. doi:10.1086/499575. Bibcode: 2006ApJ...639.1238R.
46. ↑ C. A. Trujillo; M. E. Brown (June 2003). "The Caltech Wide Area Sky Survey". Earth, Moon, and Planets 112 (1–4): 92–99. doi:10.1023/B:MOON.0000031929.19729.a1. Bibcode: 2003EM&P...92...99T.
47. ↑ Brown, M. E.; Trujillo, C.; Rabinowitz, D. L. (2004). "Discovery of a candidate inner Oort cloud planetoid". The Astrophysical Journal 617 (1): 645–649. doi:10.1086/422095. Bibcode: 2004ApJ...617..645B.
48. ↑ Schwamb, M. E.; Brown, M. E.; Rabinowitz, D. L. (2008). "Constraints on the distant population in the region of Sedna". American Astronomical Society, DPS Meeting #40, #38.07 40: 465. Bibcode: 2008DPS....40.3807S.
49. ↑ Muñoz-Gutiérrez, Marco A.; Peimbert, Antoni; Lehner, Matthew J.; Wang, Shiang-Yu (October 2021). "Long-term Dynamical Stability in the Outer Solar System. I. The Regular and Chaotic Evolution of the 34 Largest Trans-Neptunian Objects". The Astronomical Journal 162 (4): 164. doi:10.3847/1538-3881/ac1102. Bibcode: 2021AJ....162..164M.
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53. ↑ 53.0 53.1 53.2 Stansberry, J.; Grundy, W.; Brown, M.; Cruikshank, D.; Spencer, J.; Trilling, D.; Margot, J-L. (2008). "Physical Properties of Kuiper Belt and Centaur Objects: Constraints from Spitzer Space Telescope". The Solar System Beyond Neptune (University of Arizona Press): 161. Bibcode: 2008ssbn.book..161S.
54. ↑ Alexandra C. Lockwood; Michael E. Brown; John Stansberry (2014). "The size and shape of the oblong dwarf planet Haumea". Earth, Moon, and Planets 111 (3–4): 127–137. doi:10.1007/s11038-014-9430-1. Bibcode: 2014EM&P..111..127L.
55. ↑ 55.0 55.1 Brown, M. E.; Bouchez, A. H.; Rabinowitz, D.; Sari, R.; Trujillo, C. A.; Van Dam, M.; Campbell, R.; Chin, J. et al. (2005). "Keck Observatory Laser Guide Star Adaptive Optics Discovery and Characterization of a Satellite to the Large Kuiper Belt Object 2003 EL61". Astrophysical Journal Letters 632 (1): L45–L48. doi:10.1086/497641. Bibcode: 2005ApJ...632L..45B. http://authors.library.caltech.edu/34486/1/1538-4357_632_1_L45.pdf. Retrieved 2018-11-04.
56. ↑ Lacerda, P.; Jewitt, D. C. (2007). "Densities of Solar System Objects from Their Rotational Light Curves". Astronomical Journal 133 (4): 1393–1408. doi:10.1086/511772. Bibcode: 2007AJ....133.1393L.
57. ↑ Lellouch, E.Expression error: Unrecognized word "etal". (2010). ""TNOs are cool": A survey of the trans-Neptunian region II. The thermal lightcurve of (136108) Haumea". Astronomy and Astrophysics 518: L147. doi:10.1051/0004-6361/201014648. Bibcode: 2010A&A...518L.147L.
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63. ↑ P. Lacerda; D. Jewitt; N. Peixinho (2008). "High-Precision Photometry of Extreme KBO 2003 EL61". Astronomical Journal 135 (5): 1749–1756. doi:10.1088/0004-6256/135/5/1749. Bibcode: 2008AJ....135.1749L.
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67. ↑ Kondratyev, B. P.; Kornoukhov, V. S. (October 2020). "Secular Evolution of Rings around Rotating Triaxial Gravitating Bodies". Astronomy Reports 64 (10): 870–875. doi:10.1134/S1063772920100030. Bibcode: 2020ARep...64..870K.
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71. ↑ K. M. Barkume; M. E. Brown; E. L. Schaller (2006). "Water Ice on the Satellite of Kuiper Belt Object 2003 EL61". Astrophysical Journal Letters 640 (1): L87–L89. doi:10.1086/503159. Bibcode: 2006ApJ...640L..87B.
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73. ↑ 73.0 73.1 Ragozzine, D.; Brown, M. E.; Trujillo, C. A.; Schaller, E. L. (2008). "Orbits and Masses of the 2003 EL61 Satellite System". AAS DPS conference 2008. 40. 462. Bibcode: 2008DPS....40.3607R.
74. ↑ Dumas, C.; Carry, B.; Hestroffer, D.; Merlin, F. (2011). "High-contrast observations of (136108) Haumea". Astronomy & Astrophysics 528: A105. doi:10.1051/0004-6361/201015011. Bibcode: 2011A&A...528A.105D. https://www.aanda.org/articles/aa/full_html/2011/04/aa15011-10/aa15011-10.html. Retrieved 24 August 2024.
75. ↑ "IAU Circular 8949". International Astronomical Union. 17 September 2008. http://www.cfa.harvard.edu/~fabrycky/EL61/.
76. ↑ 76.0 76.1 76.2 "Mutual events of Haumea and Namaka". http://web.gps.caltech.edu/~mbrown/2003EL61/mutual/.
77. ↑ L.-A. A. McFadden; P. R. Weissman; T. V. Johnson (2007). Encyclopedia of the Solar System. Academic Press. ISBN 978-0-12-088589-3. https://books.google.com/books?id=G7UtYkLQoYoC&q=mutual+event+pluto&pg=PA545.
78. ↑ 78.0 78.1 Fabrycky, D. C.; Holman, M. J.; Ragozzine, D.; Brown, M. E.; Lister, T. A.; Terndrup, D. M.; Djordjevic, J.; Young, E. F. et al. (2008). "Mutual Events of 2003 EL61 and its Inner Satellite". AAS DPS conference 2008. 40. 462. Bibcode: 2008DPS....40.3608F.
79. ↑ M. Brown (18 May 2008). "Moon shadow Monday (fixed)". Mike Brown's Planets. http://www.mikebrownsplanets.com/2008/05/moon-shadow-monday-fixed.html.
80. ↑ Bortoletto, A.; Saito, R. K. (2010). "Observing mutual events of the trans-Neptunian object Haumea and Namaka from Brazil". Proceedings of the International Astronomical Union 269: 189–192. doi:10.1017/S1743921310007404. Bibcode: 2010IAUS..269..189B. https://articles.adsabs.harvard.edu//full/2010IAUS..269..189B/0000189.000.html. Retrieved 24 August 2024.
81. ↑ Müller, T.; Kiss, Cs; Ali-Lagoa, V.; Ortiz, J. L.; Lellouch, E.; Santos-Sanz, P.; Fornasier, S.; Marton, G. et al. (2018-11-23), "Haumea's thermal emission revisited in the light of the occultation results", Icarus 334: 39–51, doi:10.1016/j.icarus.2018.11.011, http://arxiv.org/abs/1811.09476, retrieved 2025-12-30
82. ↑ Fernández-Valenzuela, Estela; Ortiz, Jose Luis; Holler, Bryan J.; Sicardy, Bruno; Rommel, Flavia L.; Vara-Lubiano, Mónica; Morales, Nicolas; Vachier, Frederic et al. (December 2025). "Accurate geometric albedo, shape, and size of Hi'iaka from a stellar occultation" (in en). Nature Communications 16 (1): 10926. doi:10.1038/s41467-025-65749-1. ISSN 2041-1723. PMID 41326341. PMC 12686452. Bibcode: 2025NatCo..1610926F. https://ui.adsabs.harvard.edu/abs/2025NatCo..1610926F/abstract.
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86. ↑ Proudfoot, Benjamin; Ragozzine, Darin (May 2019). "Modeling the Formation of the Family of the Dwarf Planet Haumea". The Astronomical Journal 157 (6): 230. doi:10.3847/1538-3881/ab19c4. Bibcode: 2019AJ....157..230P.
87. ↑ Proudfoot, Benjamin; Fernández-Valenzuela, Estela; Stansberry, John; Kiss, Csaba; Ragozzine, Darin; Fraser, Wesley; Pike, Rosemary; Pinilla-Alonso, Noemi (December 2024). "A Near-infrared Survey of Candidate Haumea Family Members". The Astronomical Journal 168 (6): 269. doi:10.3847/1538-3881/ad864e. Bibcode: 2024AJ....168..269P.
88. ↑ 88.0 88.1 Schlichting, H. E.; Sari, R. (2009). "The Creation of Haumea's Collisional Family". The Astrophysical Journal 700 (2): 1242–1246. doi:10.1088/0004-637X/700/2/1242. Bibcode: 2009ApJ...700.1242S.
89. ↑ 89.0 89.1 89.2 Levison, H. F.; Morbidelli, A.; Vokrouhlický, D.; Bottke, W. F. (2008). "On a Scattered Disc Origin for the 2003 EL61 Collisional Family—an Example of the Importance of Collisions in the Dynamics of Small Bodies". Astronomical Journal 136 (3): 1079–1088. doi:10.1088/0004-6256/136/3/1079. Bibcode: 2008AJ....136.1079L.
90. ↑ McGranaghan, R.; Sagan, B.; Dove, G.; Tullos, A.; Lyne, J. E.; Emery, J. P. (2011). "A Survey of Mission Opportunities to Trans-Neptunian Objects". Journal of the British Interplanetary Society 64: 296–303. Bibcode: 2011JBIS...64..296M.
91. ↑ 91.0 91.1 Poncy, Joel; Fontdecaba Baiga, Jordi; Feresinb, Fred; Martinota, Vincent (2011). "A preliminary assessment of an orbiter in the Haumean system: How quickly can a planetary orbiter reach such a distant target?". Acta Astronautica 68 (5–6): 622–628. doi:10.1016/j.actaastro.2010.04.011. Bibcode: 2011AcAau..68..622P.
92. ↑ Paul Gilster: Fast Orbiter to Haumea . Centauri Dreams—The News of the Tau Zero Foundation. 14 July 2009, retrieved 15 January 2011

## External links

* (136108) Haumea, Hiʻiaka, and Namaka at Johnston's Archive.com (updated 21 September 2014)
* International Year of Astronomy 2009 podcast: Dwarf Planet Haumea (Darin Ragozzine)
* Haumea as seen on June 10, 2011 by Mike Brown using the 4.20 m (165 in) WHT / ~0:30–3:30 dip in the brightness of Haumea+Namaka comes when Namaka crosses Haumea (Hiʻiaka, the outer moon, is blended in the images, but it rotates every 4.5 hr and adds a little variation)
* Animation of Haumea's intermittent 7:12 resonance with Neptune over the next 3.5 million years

* v
* t
* e

Haumea

Moons and rings|

* Hiʻiaka
* Namaka
* Rings of Haumea

Classification|

* Dwarf planet
* Definition of planet
* 2006 definition of planet
* Kuiper belt
* Cubewano
* Trans-Neptunian object

Collisional family|

* (19308) 1996 TO66
* (24835) 1995 SM55
* (55636) 2002 TX300
* (86047) 1999 OY3
* (120178) 2003 OP32
* (145453) 2005 RR43
* (308193) 2005 CB79
* (386723) 2009 YE7
* (416400) 2003 UZ117
* 2003 SQ317

Controversy|

* José Luis Ortiz Moreno
* Michael E. Brown

Articles related to Haumea

* v
* t
* e

Solar System

* Sun
* Mercury
* Venus
* Earth
* Mars
* Ceres
* Jupiter
* Saturn
* Uranus
* Neptune
* Pluto
* Haumea
* Makemake
* Eris

| Planets|

* Terrestrial planets
* Mercury
* Venus
* Earth
* Mars

* Giant planets
* Jupiter
* Saturn
* Uranus
* Neptune

* Dwarf planets
* Ceres
* Pluto
* Haumea
* Makemake
* Eris

|

Rings|

* Jovian
* Saturnian (Rhean)
* Charikloan
* Chironean
* Uranian
* Neptunian
* Haumean

Moons|

* Terrestrial
* Moon
* other near-Earth objects
* Martian
* Phobos
* Deimos
* Jovian
* Ganymede
* Callisto
* Io
* Europa
* all 79
* Saturnian
* Titan
* Rhea
* Iapetus
* Dione
* Tethys
* Enceladus
* Mimas
* Hyperion
* Phoebe
* all 82
* Uranian
* Titania
* Oberon
* Umbriel
* Ariel
* Miranda
* all 27
* Neptunian
* Triton
* Proteus
* Nereid
* all 14
* Plutonian
* Charon
* Nix
* Hydra
* Kerberos
* Styx
* Eridian
* Dysnomia
* Haumean
* Hiʻiaka
* Namaka
* Makemakean
* S/2015 (136472) 1

Exploration
(outline)|

* Colonization
* Discovery
* astronomy
* historical models
* timeline
* Human spaceflight
* space stations
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* list

* Mercury
* Venus
* Moon
* mining
* Mars
* Ceres
* Asteroids
* mining
* Comets
* Jupiter
* Saturn
* Uranus
* Neptune
* Pluto
* Deep space

Hypothetical
objects|

* Fifth giant
* Nemesis
* Phaeton
* Planet Nine
* Planet V
* Planet X
* Theia
* Tyche
* Vulcan
* Vulcanoids
* Subsatellites

Lists|

* Comets
* Dwarf planets (possible)
* Gravitationally rounded objects
* Minor planets
* names
* Natural satellites
* Solar System models
* Solar System objects
* by size
* by discovery date

| Small Solar
System bodies|

* Comets
* Damocloids
* Meteoroids
* Minor planets
* moons
* Planetesimal

* Mercury-crossers
* Venus-crossers
* Venus trojans
* Near-Earth objects
* Earth-crossers
* Earth trojans
* Mars-crossers
* Mars trojans

* Asteroid belt
* Asteroids
* Ceres
* Pallas
* Juno
* Vesta
* first 1000
* families
* exceptional
* Kirkwood gap
* Main-belt comets

* Jupiter-crossers
* Jupiter trojans
* Centaurs
* Saturn-crossers
* Uranus-crossers
* Uranus trojans
* Neptune-crossers
* Neptune trojans
* Cis-Neptunian objects
* Trans-Neptunian objects

* Plutoids
* Kuiper belt
* Cubewanos
* Plutinos
* Detached objects
* Hills cloud
* Oort cloud
* Scattered disc
* Sednoids

|

Formation
and evolution|

* Accretion
* Accretion disk
* Asteroid belt
* Circumplanetary disk
* Circumstellar disc
* Circumstellar envelope
* Cosmic dust
* Debris disk
* Detached object
* Disrupted planet
* Excretion disk
* Exoplanetary Circumstellar Environments and Disk Explorer
* Exozodiacal dust
* Extraterrestrial materials
* Extraterrestrial sample curation
* Giant-impact hypothesis
* Gravitational collapse
* Hills cloud
* Interplanetary dust cloud
* Interplanetary medium
* Interplanetary space
* Interstellar cloud
* Interstellar dust
* Interstellar medium
* Interstellar space
* Kuiper belt
* List of interstellar and circumstellar molecules
* Merging stars
* Molecular cloud
* Nebular hypothesis
* Oort cloud
* Outer space
* Planetary migration
* Planetary system
* Planetesimal
* Planet formation
* Protoplanetary disk
* Ring system
* Rubble pile
* Sample-return mission
* Scattered disc
* Star formation

* Outline of the Solar System
*   *   *

Solar System → Local Interstellar Cloud → Local Bubble → Gould Belt → Orion Arm → Milky Way → Milky Way subgroup → Local Group → Local Sheet → Virgo Supercluster → Laniakea Supercluster → Observable universe → Universe
Each arrow (→) may be read as "within" or "part of".

* v
* t
* e

Moons of likely dwarf planets

IAU-named
dwarf planets|

| Pluto| Haumea| Makemake| Eris

|
|
|

* Charon
* Styx
* Nix
* Kerberos
* Hydra

* ring
* Namaka
* Hiʻiaka

* MK2

* Dysnomia

Other possible
dwarf planets|

| Orcus| Quaoar| Gonggong| Salacia| Varda

|
|
|
|

* Vanth

* Weywot

* Xiangliu

* Actaea

* Ilmarë

* v
* t
* e

Planetary rings

Planets|

* Rings of Jupiter
* Rings of Saturn
* Rings of Uranus
* Rings of Neptune
* Rings of exoplanets

Other bodies|

* Rings of Chariklo
* Rings of Chiron
* Rings of Rhea
* Rings of Haumea

Solar|

* Asteroid belt
* Kuiper belt

Related topics|

* Gas torus

* v
* t
* e

Minor planets navigator

* (136107) 2003 EY58
* (136108) Haumea
* (136109) 2003 FA22

* v
* t
* e

Trans-Neptunian objects

TNO classes|

* Cubewanos
* Scattered-disc objects
* Detached objects
* Resonant objects
* Neptune trojans
* Plutinos
* Twotinos
* TNO moons

Dwarf planets (moons)|

* Pluto
* Charon
* Styx
* Nix
* Kerberos
* Hydra
* Haumea
* Namaka
* Hiʻiaka
* Makemake
* S/2015 (136472) 1
* Eris
* Dysnomia

Sednoids|

* 90377 Sedna
* 2012 VP113
* 2015 TG387

* v
* t
* e

Dwarf planets

* List of possible dwarf planets
* Former dwarf planets
* Phoebe
* Triton
* Vesta
* Mesoplanet
* Planemo

Asteroid belt|

| IAU|

* Ceres

|

Possible|

* Hygiea
* Interamnia

Centaurs|

| Possible|

* Ceto
* Chariklo
* Chiron
* 1995 SN55
* 2010 TY53

|

Plutinos|

| IAU|

* Pluto

|

Possible|

* Huya
* Ixion
* Orcus
* 2001 QF298
* 2002 VR128
* 2002 XV93
* 2003 AZ84
* 2003 UZ413
* 2003 VS2
* 2007 JH43

Twotinos|

| Possible|

* 2002 WC19

|

Cubewanos|

| IAU|

* Makemake

|

Possible|

* Altjira
* Chaos
* Praamzius
* Quaoar
* Rhadamanthus
* Salacia
* Sila–Nunam
* Varda
* Varuna
* 1998 SN165
* 2002 AW197
* 2002 CY248
* 2002 KX14
* 2002 MS4
* 2002 TX300
* 2002 UX25
* 2003 OP32
* 2003 QW90
* 2004 GV9
* 2004 NT33
* 2004 PF115
* 2004 TY364
* 2004 UX10
* 2005 RN43
* 2005 RR43
* 2005 UQ513
* 2007 JJ43
* 2010 FX86
* 2010 VR11

Scattered disc|

| IAU|

* Eris

|

Possible|

* Dziewanna
* Gǃkúnǁʼhòmdímà
* 1996 GQ21
* 1996 TL66
* 1999 CC158
* 2001 UR163
* 2002 TC302
* 2004 XA192
* 2005 QU182
* 2005 RM43
* 2006 QH181
* 2007 OR10
* 2008 OG19
* 2010 KZ39
* 2010 RE64
* 2010 RF43
* 2010 TJ
* 2010 VZ98
* 2012 HH2
* 2013 FY27
* 2018 VG18

Detached objects|

| Possible|

* 1995 TL8
* 2000 CR105
* 2003 FY128
* 2003 QX113
* 2004 VN112
* 2004 XR190
* 2005 TB190
* 2008 ST291
* 2010 GB174

|

Sednoids|

| Possible|

* Sedna
* 2015 TG387
* 2012 VP113

|

Other / unknown
resonances|

| IAU|

* Haumea

|

Possible|

* FarFarOut
* V774104
* 1999 CD158
* 1999 DE9
* 1999 KR16
* 2000 YW134
* 2001 YH140
* 2002 XW93
* 2010 VK201
* 2011 FW62
* 2011 GM27
* 2013 FZ27
* 2014 UM33

* Category

* v
* t
* e

2017 in space

* « 2016

2018 »

Impact events|

* Bolides in 2017
* 2017 China bolide

Selected NEOs|

* Asteroid close approaches
* 2012 TC4
* 2013 SY99 (announced)
* 2017 AG13
* 2014 JO25
* 2016 WF9
* 2017 BQ6
* 2017 BS5
* 2017 SX17
* 3122 Florence
* C/2015 ER61 (PANSTARRS)

Exoplanets |

* HATS-36b
* KELT-18b
* Kepler-80g
* Kepler-90i
* LHS 1140 b
* Luyten b
* NGTS-1b
* OGLE-2016-BLG-1190Lb
* OGLE-2016-BLG-1195Lb
* Ross 128 b
* TRAPPIST-1e
* TRAPPIST-1f
* TRAPPIST-1g
* TRAPPIST-1h
* WASP-107b

Discoveries|

* GW170104
* GW170608
* GW170814
* GW170817
* Ring of Haumea
* IGR J17329-2731
* ʻOumuamua
* RZ Piscium
* ULAS J1342+0928
* Saraswati Supercluster

Space exploration|

* Cassini retirement

* Category:2016 in space — Category:2017 in space — Category:2018 in space

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