Haumea
Sidereal rotation period | 3.915341±0.000005 h[16] (0.163139208 d) | |
≈ 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 | |
Temperature | < 50 K[20] | |
17.3 (opposition)[23][24] | ||
0.428±0.011 (V-band) [16] · 0.2 [9] |
Haumea (
Haumea's mass is about one-third that of
History
Discovery
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 December 28, 2004, on images they had taken on May 6, 2004. On July 20, 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 March 7–10, 2003.[27] Ortiz emailed the Minor Planet Center with their discovery on the night of July 27, 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.
These 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 July 29. 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] Precovery images of Haumea have been identified back to March 22, 1955.[9]
IAU protocol is that discovery credit for a
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 December 28, 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 July 29, 2005, Haumea was given the provisional designation 2003 EL61, based on the date of the Spanish discovery image. On September 7, 2006, it was numbered and admitted into the official minor planet catalog as (136108) 2003 EL61.
Following
The proposal by the Ortiz team, Ataecina, did not meet IAU naming requirements, because the names of
Orbit
Haumea has an
With a
Possible resonance with Neptune
Haumea is thought to be in an intermittent 7:12
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.
The plane of Haumea's
Physical characteristics
Size, shape, and composition
The size of a Solar System object can be deduced from its
The rotation and amplitude of Haumea's
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.[15][53] Several ellipsoid-model calculations of Haumea's dimensions have been made. The first model produced after Haumea's discovery was calculated from
−58 km.[56]
However the observations of a
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
Haumea is as bright as snow, with an albedo in the range of 0.6–0.8, consistent with crystalline ice.
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
In addition to the large fluctuations in Haumea's light curve due to the body's shape, which affect all
Ring
A stellar occultation observed on January 21, 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][64] 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][65] 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
Satellites
Two small satellites have been discovered orbiting Haumea, (136108) Haumea I Hiʻiaka and (136108) Haumea II 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,[67] was discovered January 26, 2005.[53] 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.[68] 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.[69] 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 June 30, 2005,
At present, the orbits of the Haumean moons appear almost exactly edge-on from Earth, with Namaka periodically
Name | Diameter (km)[78][79] | Semi-major axis (km)[80] | Mass (kg)[80] | Discovery date[78][81] |
---|---|---|---|---|
Haumea | 2 322 × 1,704 × 1,026 | (4.006 ± 0.040) × 1021 | March 7, 2003[81] | |
Hiʻiaka | ≈ 310 | 49 880 | (1.79 ± 0.11) x 1019 | January 26, 2005 |
Namaka | ≈ 170 | 25 657 | (1.79 ± 1.48) x 1018 | June 30, 2005 |
Collisional family
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).[6] 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.[82] 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.[82]
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.[83] 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.[83] 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.[83]
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 very early in the Solar System's history.[6]
Exploration
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]
Joel Poncy and colleagues calculated that a flyby mission to Haumea could take 14.25 years using a gravity assist at Jupiter, based on a launch date of 25 September 2025. Haumea would be 48.18 AU from the Sun when the spacecraft arrives. A flight time of 16.45 years can be achieved with launch dates on 1 November 2026, 23 September 2037 and 29 October 2038.[84] Haumea could become a target for an exploration mission,[85] and an example of this work is a preliminary study on a probe to Haumea and its moons (at 35–51 AU).[86] Probe mass, power source, and propulsion systems are key technology areas for this type of mission.[85]
See also
- Astronomical naming conventions
- Clearing the neighbourhood
- International Astronomical Union
- Planets beyond Neptune
- List of Solar System objects most distant from the Sun
Notes
- ^ how-MAY-ə, with three syllables according to the English pronunciation in Hawaii,[1] or HAH-oo-MAY-ə with four syllables according to Brown's students.[2][3]
- semi-major axisa: .
- ^ a b c d e f Best fit physical model assuming hydrostatic equilibrium for Haumea.[11]
- ^ Occultation-derived model based on the assumption Haumea's ring does not contribute to its total brightness.[12]
- ^ a b Occultation-derived model based on the upper-limit assumption that Haumea's ring contributes 5% to its total brightness.[12]
- 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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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