Haumea

Source: Wikipedia, the free encyclopedia.

136108 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 (

Caltech at the Palomar Observatory in the United States and disputably also in 2005 by a team headed by José Luis Ortiz Moreno at the Sierra Nevada Observatory in Spain. On September 17, 2008, it was named after Haumea, the Hawaiian goddess of childbirth, 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
.

Haumea's mass is about one-third that of

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. 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), are thought to be the consequences of a giant collision, which left Haumea the largest member of a collisional family that includes several large trans-Neptunian objects and Haumea's two known moons, Hiʻiaka and Namaka
.

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

chthonic deity, it would have been appropriate for a plutino
, which Haumea is 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 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

Mauna Kea Observatory is located. 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

Ataecina § Dwarf planet
.)

Planetary symbols are no longer much used in astronomy. A Haumea symbol 🝻 is included in Unicode as U+1F77B:[38] it 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

aphelion in early 1992, and is currently more than 50 AU from the Sun.[23] It will come to perihelion in 2133.[10] 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

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.

Possible resonance with Neptune

rotating frame, with Neptune stationary (see 2 Pallas for an example of non-librating)
The libration angle of Haumea's weak 7:12 resonance with Neptune, , over the next 5 million years

Haumea is thought to be in an intermittent 7:12

ascending node
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.[5] As this is not a simple resonance, Marc Buie qualifies it as non-resonant.[49]

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.

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

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.[51] 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

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.[15][53] Several ellipsoid-model calculations of Haumea's dimensions have been made. The first model produced after Haumea's discovery was calculated from

Herschel Space Telescope together with the older Spitzer Telescope measurements yielded a new estimate of the equivalent diameter of Haumea—about 1300 km.[55] 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
.[56]

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 rapidly rotates in just under 4 hours, causing it to be elongated. 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,[51] 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

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.

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.[59]
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.[60]

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.[61][62] 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.[50][63]
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 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

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.[66]

Satellites

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 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,

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 is inclined 13° from the larger moon, which perturbs its orbit.[71]
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.[72]

At present, the orbits of the Haumean moons appear almost exactly edge-on from Earth, with Namaka periodically

the late 1980s with Pluto and Charon.[75] The tiny change in brightness of the system during these occultations will require at least a medium-aperture professional telescope for detection.[74][76] Hiʻiaka last occulted Haumea in 1999, a few years before discovery, and will not do so again for some 130 years.[77] However, in a situation unique among regular satellites, Namaka's orbit is being greatly torqued by Hiʻiaka, which preserved the viewing angle of Namaka–Haumea transits for several more years.[71][74][76]

Haumean system
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

New Horizons
spacecraft in 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]

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

Notes

  1. ^ how-MAY, with three syllables according to the English pronunciation in Hawaii,[1] or HAH-oo-MAY with four syllables according to Brown's students.[2][3]
  2. semi-major axis
    a:  .
  3. ^ a b c d e f 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. ^ a b Occultation-derived model based on the upper-limit assumption that Haumea's ring contributes 5% to its total brightness.[12]
  6. 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.

References

  1. ^ New dwarf planet named for Hawaiian goddess Archived 2015-12-08 at the Wayback Machine (HeraldNet, September 19, 2008)
  2. ^ "DPS08 Webstreaming". Archived from the original on 2009-01-06. Retrieved 2009-02-14.
  3. ^ "365 Days of Astronomy". Archived from the original on 2012-02-20. Retrieved 2009-04-11.
  4. ^ "MPEC 2010-H75: Distant Minor Planets (2010 May 14.0 TT)". Minor Planet Center. 2010-04-10. Archived from the original on 2014-07-16. Retrieved 2010-07-02.
  5. ^ a b
    Marc W. Buie (2008-06-25). "Orbit Fit and Astrometric record for 136108". Southwest Research Institute (Space Science Department). Archived
    from the original on 2011-05-18. Retrieved 2008-10-02.
  6. ^ a b c Ragozzine, D.; Brown, M. E. (2007). "Candidate Members and Age Estimate of the Family of Kuiper Belt Object 2003 EL61".
    S2CID 8387493
    .
  7. ^ E.g. Giovanni Vulpetti (2013) Fast Solar Sailing, p. 333.
  8. ^ "(136108) Haumea = 2003 EL61". Minor Planet Center. International Astronomical Union. Archived from the original on 24 July 2021. Retrieved 14 March 2021.
  9. ^ a b c d "Jet Propulsion Laboratory Small-Body Database Browser: 136108 Haumea (2003 EL61)" (2019-08-26 last obs). NASA's Jet Propulsion Laboratory. Archived from the original on 2020-07-11. Retrieved 2020-02-20.
  10. ^ a b "Horizons Batch for Haumea at perihelion around 1 June 2133". JPL Horizons (Perihelion occurs when rdot flips from negative to positive. The JPL SBDB generically (incorrectly) lists an unperturbed two-body perihelion date in 2132). Jet Propulsion Laboratory. Archived from the original on 2021-09-13. Retrieved 13 September 2021.
  11. ^ a b c d Dunham, E. T.; Desch, S. J.; Probst, L. (April 2019). "Haumea's Shape, Composition, and Internal Structure". The Astrophysical Journal. 877 (1): 11.
    S2CID 90262114
    .
  12. ^ (PDF) from the original on 2020-11-07. Retrieved 2020-08-19.
  13. ^ "Ellipsoid surface area: 8.13712×10^6 km2". wolframalpha.com. 20 December 2019. Archived from the original on 25 July 2020. Retrieved 20 December 2019.
  14. ^ "Ellipsoid volume: 1.98395×10^9 km3". wolframalpha.com. 20 December 2019. Archived from the original on 25 July 2020. Retrieved 20 December 2019.
  15. ^ a b c Ragozzine, D.; Brown, M. E. (2009). "Orbits and Masses of the Satellites of the Dwarf Planet Haumea = 2003 EL61". The Astronomical Journal. 137 (6): 4766–4776.
    S2CID 15310444
    .
  16. ^ .
  17. ^ a b c d 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. .
  18. ^ "Coordinate Transformation & Galactic Extinction Calculator". NASA/IPAC Extragalactic Database. California Institute of Technology. Archived from the original on 22 January 2023. Retrieved 11 February 2023. 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. ^ . 95.
  20. ^ a b c d e f g
    S2CID 118938812
    .
  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.
    S2CID 62880843
    .
  22. ^ a b 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.
    S2CID 117167835
    .
  23. ^ a b c "AstDys (136108) Haumea Ephemerides". Department of Mathematics, University of Pisa, Italy. Archived from the original on 2011-06-29. Retrieved 2009-03-19.
  24. ^ "HORIZONS Web-Interface". NASA Jet Propulsion Laboratory Solar System Dynamics. Archived from the original on 2008-07-18. Retrieved 2008-07-02.
  25. ^ a b c "IAU names fifth dwarf planet Haumea". IAU Press Release. 2008-09-17. Archived from the original on 2011-07-02. Retrieved 2008-09-17.
  26. ^ Michael E Brown. "The electronic trail of the discovery of 2003 EL61". Caltech. Archived from the original on 2006-09-01. Retrieved 2006-08-16.
  27. ^ a b c Pablo Santos Sanz (2008-09-26). "La historia de Ataecina vs Haumea" (in Spanish). infoastro.com. Archived from the original on 2008-09-29. Retrieved 2008-09-29.
  28. ^ Michael E. Brown. How I Killed Pluto and Why It Had It Coming, chapter 9: "The Tenth Planet"
  29. ^ Jeff Hecht (2005-09-21). "Astronomer denies improper use of web data". New Scientist.com. Archived from the original on 2011-03-13. Retrieved 2009-01-12.
  30. ^ a b "Dwarf Planets and their Systems". US Geological Survey Gazetteer of Planetary Nomenclature. Archived from the original on 2011-06-29. Retrieved 2008-09-17.
  31. ^ Rachel Courtland (2008-09-19). "Controversial dwarf planet finally named 'Haumea'". NewScientistSpace. Archived from the original on 2008-09-19. Retrieved 2008-09-19.
  32. ^ "Santa et al". NASA Astrobiology Magazine. 2005-09-10. Archived from the original on 2006-04-26. Retrieved 2008-10-16.{{cite web}}: CS1 maint: unfit URL (link)
  33. ^ "Naming of Astronomical Objects: Minor planets". International Astronomical Union. Archived from the original on 2008-12-16. Retrieved 2008-11-17.
  34. ^ Mike Brown (2008-09-17). "Dwarf planets: Haumea". Caltech. Archived from the original on 2008-09-15. Retrieved 2008-09-18.
  35. ^ from the original on 2023-02-08. Retrieved 2020-11-11.
  36. ^ a b "News Release – IAU0807: IAU names fifth dwarf planet Haumea". International Astronomical Union. 2008-09-17. Archived from the original on 2009-07-08. Retrieved 2008-09-18.
  37. ^ (PDF) from the original on 2020-05-04. Retrieved 2019-07-14.
  38. ^ "Proposed New Characters: The Pipeline". Archived from the original on 2022-01-29. Retrieved 2022-01-29.
  39. ^ Miller, Kirk (26 October 2021). "Unicode request for dwarf-planet symbols" (PDF). unicode.org. Archived (PDF) from the original on 23 March 2022. Retrieved 6 August 2022.
  40. ^ JPL/NASA (April 22, 2015). "What is a Dwarf Planet?". Jet Propulsion Laboratory. Archived from the original on 2021-01-19. Retrieved 2021-09-24.
  41. ^ Anderson, Deborah (4 May 2022). "Out of this World: New Astronomy Symbols Approved for the Unicode Standard". unicode.org. The Unicode Consortium. Archived from the original on 6 August 2022. Retrieved 6 August 2022.
  42. ^ a b c Michael E. Brown. "The largest Kuiper belt objects" (PDF). Caltech. Archived (PDF) from the original on 2008-10-01. Retrieved 2008-09-19.
  43. S2CID 15167447
    .
  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.
    S2CID 12641453
    .
  45. ^ a b c d e f g h 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".
    S2CID 11484750
    .
  46. ^ C. A. Trujillo & M. E. Brown (June 2003). "The Caltech Wide Area Sky Survey". Earth, Moon, and Planets. 112 (1–4): 92–99.
    S2CID 189905639
    .
  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.
    S2CID 7738201
    .
  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. .
  49. ^ "Orbit and Astrometry for 136108". www.boulder.swri.edu. Archived from the original on 2020-07-13. Retrieved 2020-07-14.
  50. ^ a b Agence France-Presse (2009-09-16). "Astronomers get lock on diamond-shaped Haumea". European Planetary Science Congress in Potsdam. News Limited. Archived from the original on 2009-09-23. Retrieved 2009-09-16.
  51. ^ a b c 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. .
  52. ^ 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.
    S2CID 18646829
    .
  53. ^ (PDF) from the original on 2017-12-02. Retrieved 2018-11-04.
  54. ^ Lacerda, P.; Jewitt, D. C. (2007). "Densities of Solar System Objects from Their Rotational Light Curves".
    S2CID 17735600
    .
  55. ^ Lellouch, E.; Kiss, C.; Santos-Sanz, P.; Müller, T. G.; Fornasier, S.; Groussin, O.; et al. (2010). ""TNOs are cool": A survey of the trans-Neptunian region II. The thermal lightcurve of (136108) Haumea".
    S2CID 119223894
    .
  56. ^ Fornasier, S.; Lellouch, E.; Müller, T.; Santos-Sanz, P.; Panuzzo, P.; Kiss, C.; Lim, T.; Mommert, M.; (PDF) from the original on 2014-12-05.
  57. ^ "Charon: An ice machine in the ultimate deep freeze" (Press release). Gemini Observatory. 17 July 2007. Archived from the original on 7 June 2011. Retrieved 2007-07-18.
  58. ^ Brown, M. E.; Schaller, E. L.; Roe, H. G.; Rabinowitz, D. L.; Trujillo, C. A. (2006). "Direct measurement of the size of 2003 UB313 from the Hubble Space Telescope" (PDF). (PDF) from the original on 2008-09-10.
  59. ^ Pinilla-Alonso, N.; Brunetto, R.; Licandro, J.; Gil-Hutton, R.; Roush, T. L.; Strazzulla, G. (2009). "Study of the Surface of 2003 EL61, the largest carbon-depleted object in the trans-neptunian belt".
    S2CID 15139257
    .
  60. ^ Tegler, S. C.; Grundy, W. M.; Romanishin, W.; Consolmagno, G. J.; Mogren, K.; Vilas, F. (2007). "Optical Spectroscopy of the Large Kuiper Belt Objects 136472 (2005 FY9) and 136108 (2003 EL61)". The Astronomical Journal. 133 (2): 526–530.
    S2CID 10673951
    .
  61. ^ P. Lacerda; D. Jewitt & N. Peixinho (2008). "High-Precision Photometry of Extreme KBO 2003 EL61".
    S2CID 115712870
    .
  62. ^ P. Lacerda (2009). "Time-Resolved Near-Infrared Photometry of Extreme Kuiper Belt Object Haumea".
    S2CID 15210854
    .
  63. ^ "Strange Dwarf Planet Has Red Spot". Space.com. 15 September 2009. Archived from the original on 21 November 2009. Retrieved 2009-11-12.
  64. ^ Surprise! Dwarf Planet Haumea Has a Ring Archived 2017-10-22 at the Wayback Machine, Sky and Telescope, October 13, 2017.
  65. ^ Kondratyev, B. P.; Kornoukhov, V. S. (October 2020). "Secular Evolution of Rings around Rotating Triaxial Gravitating Bodies". Astronomy Reports. 64 (10): 870–875. .
  66. .
  67. ^ K. Chang (20 March 2007). "Piecing Together the Clues of an Old Collision, Iceball by Iceball".
    New York Times. Archived
    from the original on 12 November 2014. Retrieved 2008-10-12.
  68. ^ (PDF) from the original on 2013-11-03. Retrieved 2011-10-19.
  69. ^ K. M. Barkume; M. E. Brown & E. L. Schaller (2006). "Water Ice on the Satellite of Kuiper Belt Object 2003 EL61".
    S2CID 17831967
    .
  70. ^ Green, Daniel W. E. (1 December 2005). "Iauc 8636". Archived from the original on 12 March 2018.
  71. ^ a b 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. Bulletin of the American Astronomical Society. Vol. 40. p. 462. .
  72. ^ Ragozzine, D.; Brown, M. E. (2009). "Orbits and Masses of the Satellites of the Dwarf Planet Haumea = 2003 EL61". The Astronomical Journal. 137 (6): 4766–4776.
    S2CID 15310444
    .
  73. ^ "IAU Circular 8949". International Astronomical Union. 17 September 2008. Archived from the original on 11 January 2009. Retrieved 2008-12-06.
  74. ^ a b c "Mutual events of Haumea and Namaka". Archived from the original on 2009-02-24. Retrieved 2009-02-18.
  75. ^ L.-A. A. McFadden; P. R. Weissman; T. V. Johnson (2007). Encyclopedia of the Solar System. .
  76. ^ a b Fabrycky, D. C.; Holman, M. J.; Ragozzine, D.; Brown, M. E.; Lister, T. A.; Terndrup, D. M.; Djordjevic, J.; Young, E. F.; Young, L. A.; Howell, R. R. (2008). Mutual Events of 2003 EL61 and its Inner Satellite. AAS DPS conference 2008. Bulletin of the American Astronomical Society. Vol. 40. p. 462. .
  77. ^ M. Brown (18 May 2008). "Moon shadow Monday (fixed)". Mike Brown's Planets. Archived from the original on 1 October 2008. Retrieved 2008-09-27.
  78. ^ a b "Moons of the Dwarf Planet Haumea: Hi'iaka and Namaka - Windows to The Universe". Windows To The Universe. Archived from the original on 2021-06-28. Retrieved 2021-06-08.
  79. from the original on 2022-06-23. Retrieved 2021-07-08.
  80. ^ from the original on 2021-05-09. Retrieved 2021-07-08.
  81. ^ a b "In Depth | Haumea". NASA Solar System Exploration. Archived from the original on June 29, 2021. Retrieved July 8, 2021.
  82. ^ a b Schlichting, H. E.; Sari, R. (2009). "The Creation of Haumea's Collisional Family". The Astrophysical Journal. 700 (2): 1242–1246.
    S2CID 19022987
    .
  83. ^ a b c 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".
    S2CID 10861444
    .
  84. .
  85. ^ .
  86. ^ Paul Gilster: Fast Orbiter to Haumea Archived 2015-09-23 at the Wayback Machine. Centauri Dreams—The News of the Tau Zero Foundation. July 14, 2009, retrieved January 15, 2011

External links

This page is based on the copyrighted Wikipedia article: Haumea. Articles is available under the CC BY-SA 3.0 license; additional terms may apply.Privacy Policy