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28978 Ixion
28978 Ixion (/ɪkˈsaɪ.ən/, provisional designation 2001 KX76) is a large trans-Neptunian object and a possible dwarf planet. It is located in the Kuiper belt, a region of icy objects orbiting beyond Neptune in the outer Solar System. Ixion is classified as a plutino, a dynamical class of objects in a 2:3 orbital resonance with Neptune. It was discovered in May 2001 by astronomers of the Deep Ecliptic Survey at the Cerro Tololo Inter-American Observatory, and was announced in July 2001. The object is named after the Greek mythological figure Ixion, who was a king of the Lapiths.

In visible light, Ixion appears dark and moderately red in color due to organic compounds covering its surface. Water ice has been suspected to be present on Ixion's surface, but may exist in trace amounts hidden underneath a thick layer of organic compounds. Ixion has a measured diameter of 710 km (440 mi), making it the fourth-largest known plutino. Several astronomers have considered Ixion to be a possible dwarf planet, whereas others consider it a transitional object between irregularly-shaped small Solar System bodies and spherical dwarf planets. Ixion is currently not known to have a natural satellite, so its mass and density remain unknown.

History

Discovery

Ixion was discovered with the Víctor M. Blanco Telescope at the Cerro Tololo Observatory

Ixion was discovered on 22 May 2001 by a team of American astronomers at the Cerro Tololo Inter-American Observatory in Chile. The discovery formed part of the Deep Ecliptic Survey, a survey conducted by American astronomer Robert Millis to search for Kuiper belt objects located near the ecliptic plane using telescopes at the facilities of the National Optical Astronomy Observatory. On the night of 22 May 2001, American astronomers James Elliot and Lawrence Wasserman identified Ixion in digital images of the southern sky taken with the 4-meter Víctor M. Blanco Telescope at Cerro Tololo. Ixion was first noted by Elliot while compiling two images taken approximately two hours apart, which revealed Ixion's slow motion relative to the background stars. At the time of discovery, Ixion was located in the constellation of Scorpius.

The discoverers of Ixion noted that it appeared relatively bright for a distant object, implying that it might be rather large for a TNO. The discovery supported suggestions that there were undiscovered large trans-Neptunian objects comparable in size to Pluto. Since Ixion's discovery, numerous large trans-Neptunian objects, notably the dwarf planets Haumea, Eris, and Makemake, have been discovered; in particular, Eris is almost the same size as Pluto.

The discovery of Ixion was formally announced by the Minor Planet Center in a Minor Planet Electronic Circular on 1 July 2001. It was given the provisional designation 2001 KX76, indicating that it was discovered in the second half of May 2001. Ixion was the 1,923rd object discovered in the latter half of May, as indicated by the last letter and numbers in its provisional designation.

At the time of discovery, Ixion was thought to be among the largest trans-Neptunian objects in the Solar System, as implied by its high intrinsic brightness. These characteristics of Ixion prompted follow-up observations in order to ascertain its orbit, which would in turn improve the certainty of later size estimates of Ixion. In August 2001, a team of astronomers used the European Southern Observatory's Astrovirtel virtual observatory to automatically scan through archival precovery photographs obtained from various observatories. The team obtained nine precovery images of Ixion, with the earliest taken by the Siding Spring Observatory on 17 July 1982. These precovery images along with subsequent follow-up observations with the La Silla Observatory's 2.2-meter MPG/ESO telescope in 2001 extended Ixion's observation arc by over 18 years, sufficient for its orbit to be accurately determined and eligible for numbering by the Minor Planet Center. Ixion was given the permanent minor planet number 28978 on 2 September 2001.

Name

Ixion imaged by the MPG/ESO telescope's Wide Field Imager at the La Silla Observatory in 2001

This minor planet is named after the Greek mythological figure Ixion, in accordance with the International Astronomical Union's (IAU's) naming convention which requires plutinos (objects in a 3:2 orbital resonance with Neptune) to be named after mythological figures associated with the underworld. In Greek mythology, Ixion was the king of the legendary Lapiths of Thessaly and had married Dia, a daughter of Deioneus (or Eioneus), whom Ixion promised to give valuable bridal gifts. Ixion invited Deioneus to a banquet but instead pushed him into a pitfall of burning coals and wood, killing Deioneus. Although the lesser gods despised his actions, Zeus pitied Ixion and invited him to a banquet with other gods. Rather than being grateful, Ixion became lustful towards Zeus's wife, Hera. Zeus found out about his intentions and created the cloud Nephele in the shape of Hera, and tricked Ixion into coupling with it, fathering the race of Centaurs. For his crimes, Ixion was expelled from Olympus, blasted with a thunderbolt, and bound to a burning solar wheel in the underworld for all eternity.

The name for Ixion was suggested by E. K. Elliot, who was also involved in the naming of Kuiper belt object 38083 Rhadamanthus. The naming citation was published by the Minor Planet Center on 28 March 2002.

The usage of planetary symbols is discouraged in astronomy, so Ixion never received a symbol in the astronomical literature. There is no standard symbol for Ixion used by astrologers either. Sandy Turnbull proposed a symbol for Ixion (), which includes the initials I and X as well as depicts the solar wheel that Ixion was bound to in Tartarus. Denis Moskowitz, a software engineer in Massachusetts who designed the symbols for most of the dwarf planets, substitutes the Greek letter iota (Ι) and xi (Ξ) for I and X, creating a variant (). These symbols are occasionally mentioned on astrological websites, but are not used broadly.

Orbit and rotation

Ixion is classified as a plutino, a large population of resonant trans-Neptunian objects in a 2:3 mean-motion orbital resonance with Neptune. Thus, Ixion completes two orbits around the Sun for every three orbits that Neptune takes. At the time of Ixion's discovery, it was initially thought to be in a 3:4 orbital resonance with Neptune, which would have made Ixion closer to the Sun. Ixion orbits the Sun at an average distance of 39.8 AU (5.95 billion km; 3.70 billion mi), taking 251 years to complete a full orbit. This is characteristic of all plutinos, which have orbital periods around 250 years and semi-major axes around 39 AU.

Like Pluto, Ixion's orbit is elongated and inclined to the ecliptic. Ixion has an orbital eccentricity of 0.24 and an orbital inclination of 19.6 degrees, slightly greater than Pluto's inclination of 17 degrees. Over the course of its orbit, Ixion's distance from the Sun varies from 30 AU at perihelion (closest distance) to 49.6 AU at aphelion (farthest distance). Although Ixion's orbit is similar to that of Pluto, their orbits are oriented differently: Ixion's perihelion is below the ecliptic whereas Pluto's is above it (see right image). As of 2019, Ixion is approximately 39 AU from the Sun and is currently moving closer, approaching perihelion by 2070. Simulations by the Deep Ecliptic Survey show that Ixion can acquire a perihelion distance (qmin) as small as 27.5 AU over the next 10 million years.

The rotation period of Ixion is uncertain; various photometric measurements suggest that it displays very little variation in brightness, with a small light curve amplitude of less than 0.15 magnitudes. Initial attempts to determine Ixion's rotation period were conducted by astronomer Ortiz and colleagues in 2001 but yielded inconclusive results. Although their short-term photometric data was insufficient for Ixion's rotation period to be determined based on its brightness variations, they were able to constrain Ixion's light curve amplitude below 0.15 magnitudes. Astronomers Sheppard and Jewitt obtained similarly inconclusive results in 2003 and provided an amplitude constraint less than 0.05 magnitudes, considerably less than Ortiz's amplitude constraint. In 2010, astronomers Rousselot and Petit observed Ixion with the European Southern Observatory's New Technology Telescope and determined Ixion's rotation period to be 15.9±0.5 hours, with a light curve amplitude around 0.06 magnitudes. Galiazzo and colleagues obtained a shorter rotation period of 12.4±0.3 hours in 2016, though they calculated that there is a 1.2% probability that their result may be erroneous.

Physical characteristics

Size and brightness

Size estimates for Ixion
Year Diameter (km) Refs
2002 1055±165
2003 <804
2005 <822
2005 475±75
2005 480+152
−136
2007 ~446.3
(Spitzer 1-Band)
2007 573.1+141.9
−139.7
(Spitzer 2-Band)
2007 650+260
−220 (adopted)
2007 590±190
2013 ~549
2013 617+19
−20
2021 709.6±0.2
Comparison of the relative colors and sizes of the four largest plutinos and their moons
Different diameters for Ixion depending on its albedo

Ixion has a measured diameter of 710 km (440 mi), with an optical absolute magnitude of 3.77 and a geometric albedo (reflectivity) of 0.11. Compared to Pluto and its moon Charon, Ixion is less than one-third the diameter of Pluto and three-fifths the diameter of Charon. Ixion is the fourth-largest known plutino that has a well-constrained diameter, preceding 2003 AZ84, Orcus, and Pluto. It was the intrinsically brightest object discovered by the Deep Ecliptic Survey and is among the twenty brightest trans-Neptunian objects known according to astronomer Michael Brown and the Minor Planet Center.

Ixion was the largest and brightest Kuiper belt object found when it was discovered. Under the assumption of a low albedo, it was presumed to have a diameter around 1,200 km (750 mi), which would have made it larger than the dwarf planet Ceres and comparable in size to Charon. Subsequent observations of Ixion with the La Silla Observatory's MPG/ESO telescope along with the European Southern Observatory's Astrovirtel in August 2001 concluded a similar size around 1,200–1,400 km (750–870 mi), though under the former assumption of a low albedo.

In 2002, astronomers of the Max Planck Institute for Radio Astronomy measured Ixion's thermal emission at millimeter wavelengths with the IRAM 30m telescope and obtained an albedo of 0.09, corresponding to a diameter of 1,055 km (656 mi), consistent with previous assumptions of Ixion's size and albedo. They later reevaluated their results in 2003 and realized that their detection of Ixion's thermal emission was spurious; follow-up observations with the IRAM telescope did not detect any thermal emission within the millimeter range at frequencies of 250 GHz, implying a high albedo and consequently a smaller size for Ixion. The lower limit for Ixion's albedo was constrained at 0.15, suggesting that Ixion's diameter did not exceed 804 km (500 mi).

With space-based telescopes such as the Spitzer Space Telescope, astronomers were able to more accurately measure Ixion's thermal emissions, allowing for more accurate estimates of its albedo and size. Preliminary thermal measurements with Spitzer in 2005 yielded a much higher albedo constraint of 0.25–0.50, corresponding to a diameter range of 400–550 km (250–340 mi). Further Spitzer thermal measurements at multiple wavelength ranges (bands) in 2007 yielded mean diameter estimates around 446 km (277 mi) and 573 km (356 mi) for a single-band and two-band solution for the data, respectively. From these results, the adopted mean diameter was 650+260
−220 km (404+162
−137 mi), just beyond Spitzer's 2005 diameter constraint albeit having a large margin of error. Ixion's diameter was later revised to 617 km (383 mi), based on multi-band thermal observations by the Herschel Space Observatory along with Spitzer in 2013.

On 13 October 2020, Ixion occulted a 10th magnitude red giant star (star Gaia DR2 4056440205544338944), blocking out its light for a duration of approximately 45 seconds. The stellar occultation was observed by astronomers from seven different sites across the western United States. Of the ten participating observers, eight of them reported positive detections of the occultation. Observers from the Lowell Observatory provided highly precise measurements of the occultation chord timing, allowing for tight constraints to Ixion's diameter and possible atmosphere. An elliptical fit for Ixion's occultation profile gives projected dimensions of approximately 757 km × 685 km (470 mi × 426 mi), corresponding to a projected spherical diameter of 709.6 ± 0.2 km (440.92 ± 0.12 mi). The precise Lowell Observatory chords place an upper limit surface pressure of <2 microbars for any possible atmosphere of Ixion.

Possible dwarf planet

Astronomer Gonzalo Tancredi considers Ixion as a likely candidate as it has a diameter greater than 450 km (280 mi), the estimated minimum size for an object to achieve hydrostatic equilibrium, under the assumption of a predominantly icy composition. Ixion also displays a light curve amplitude less than 0.15 magnitudes, indicative of a likely spheroidal shape, hence why Tancredi considered Ixion as a likely dwarf planet. American astronomer Michael Brown considers Ixion to highly likely be a dwarf planet, placing it at the lower end of the "highly likely" range. However, in 2019, astronomer William Grundy and colleagues proposed that trans-Neptunian objects similar in size to Ixion, around 400–1,000 km (250–620 mi) in diameter, have not collapsed into solid bodies and are thus transitional between smaller, porous (and thus low-density) bodies and larger, denser, brighter and geologically differentiated planetary bodies such as dwarf planets. Ixion is situated within this size range, suggesting that it is at most only partially differentiated, with a porous internal structure. While Ixion's interior may have collapsed gravitationally, its surface remained uncompressed, implying that Ixion might not be in hydrostatic equilibrium and thus not a dwarf planet. However, this notion for Ixion cannot currently be tested: the object is not currently known to have any natural satellites, and thus Ixion's mass and density cannot currently be measured. Only two attempts with the Hubble Space Telescope have been made to find a satellite within an angular distance of 0.5 arcseconds from Ixion, and it has been suggested that there is a chance as high as 0.5% that a satellite may have been missed in these searches.

Spectra and surface

Comparison of sizes, albedo, and colors of various large trans-Neptunian objects with sizes of >700 km. The dark colored arcs represent uncertainties of the object's size.

The surface of Ixion is very dark and unevolved, resembling those of smaller, primitive Kuiper belt objects such as Arrokoth. In the visible spectrum, Ixion appears moderately red in color, similar to the large Kuiper belt object Quaoar. Ixion's reflectance spectrum displays a red spectral slope that extends from wavelengths of 0.4 to 0.95 μm, in which it reflects more light at these wavelengths. Longward of 0.85 μm, Ixion's spectrum becomes flat and featureless, especially at near-infrared wavelengths. In the near-infrared, Ixion's reflectance spectrum appears neutral in color and lacks apparent absorption signatures of water ice at wavelengths of 1.5 and 2 μm. Although water ice appears to be absent in Ixion's near-infrared spectrum, Barkume and colleagues have reported a detection of weak absorption signatures of water ice in Ixion's near-infrared spectrum in 2007. Ixion's featureless near-infrared spectrum indicates that its surface is covered with a thick layer of dark organic compounds irradiated by solar radiation and cosmic rays.

The red color of Ixion's surface originates from the irradiation of water- and organic-containing clathrates by solar radiation and cosmic rays, which produces dark, reddish heteropolymers called tholins that cover its surface. The production of tholins on Ixion's surface is responsible for Ixion's red, featureless spectrum as well as its low surface albedo. Ixion's neutral near-infrared color and apparent lack of water ice indicates that it has a thick layer of tholins covering its surface, suggesting that Ixion has undergone long-term irradiation and has not experienced resurfacing by impact events that may otherwise expose water ice underneath. While Ixion is generally known to have a red color, visible and near-infrared observations by the Very Large Telescope (VLT) in 2006 and 2007 paradoxically found a bluer color. This discrepancy was concluded to be an indication of heterogeneities across its surface, which may also explain the conflicting detections of water ice in various studies.

In 2003, VLT observations tentatively resolved a weak absorption feature at 0.8 μm in Ixion's spectrum, which could possibly be attributed to surface materials aqueously altered by water. However, it was not confirmed in a follow-up study by Boehnhardt and colleagues in 2004, concluding that the discrepancy between the 2003 and 2004 spectroscopic results may be the result of Ixion's heterogenous surface. In that same study, their results from photometric and polarimetric observations suggest that Ixion's surface consists of a mixture of mostly dark material and a smaller proportion of brighter, icy material. Boehnhardt and colleagues suggested a mixing ratio of 6:1 for dark and bright material as a best-fit model for a geometric albedo of 0.08. Based on combined visible and infrared spectroscopic results, they suggested that Ixion's surface consists of a mixture largely of amorphous carbon and tholins, with the following best-fit model of Ixion's surface composition: 65% amorphous carbon, 20% cometary ice tholins (ice tholin II), 13% nitrogen and methane-rich Titan tholins, and 2% water ice.

In 2005, astronomers Lorin and Rousselot observed Ixion with the VLT in attempt to search for evidence of cometary activity. They did not detect a coma around Ixion, placing an upper limit of 5.2 kilograms per second for Ixion's dust production rate.

Exploration

The New Horizons spacecraft, which successfully flew by Pluto in 2015, observed Ixion from afar using its long range imager on 13 and 14 July 2016. The spacecraft detected Ixion at magnitude 20.2 from a range of 15 AU (2.2 billion km; 1.4 billion mi), and was able to observe it from a high phase angle of 64 degrees, enabling the determination of the light scattering properties and photometric phase curve behavior of its surface.

In a study published by Ashley Gleaves and colleagues in 2012, Ixion was considered as a potential target for an orbiter mission concept, which would be launched on an Atlas V 551 or Delta IV HLV rocket. For an orbiter mission to Ixion, the spacecraft have a launch date in November 2039 and use a gravity assist from Jupiter, taking 20 to 25 years to arrive. Gleaves concluded that Ixion and Huya were the most feasible targets for the orbiter, as the trajectories required the fewest maneuvers for orbital insertion around either. For a flyby mission to Ixion, planetary scientist Amanda Zangari calculated that a spacecraft could take just over 10 years to arrive at Ixion using a Jupiter gravity assist, based on a launch date of 2027 or 2032. Ixion would be approximately 31 to 35 AU from the Sun when the spacecraft arrives. Alternatively, a flyby mission with a later launch date of 2040 would also take just over 10 years, using a Jupiter gravity assist. By the time the spacecraft arrives in 2050, Ixion would be approximately 31 to 32 AU from the Sun. Other trajectories using gravity assists from Jupiter or Saturn have been also considered. A trajectory using gravity assists from Jupiter and Saturn could take under 22 years, based a launch date of 2035 or 2040, whereas a trajectory using one gravity assist from Saturn could take at least 19 years, based on a launch date of 2038 or 2040. Using these alternative trajectories for the spacecraft, Ixion would be approximately 30 AU from the Sun when the spacecraft arrives.

Notes

  1. ^ The Minor Planet Electronic Circular published in July 2001 lists two coordinates of Ixion taken from the two recorded observations at Cerro Tololo (observatory code 806) on 22 May 2001. The time between the first and second observations is 0.08127 days, or approximately 1.95 hours. Within this time interval, Ixion has moved about 0.41 arcseconds from its original position first observed by Cerro Tololo.
  2. ^ The given equatorial coordinates of Ixion during 22 May 2001 is 16 16 06.12 and −19° 13′ 45.6″, which is close to the Scorpius constellation's coordinates around 17 and −40°.
  3. ^ In the convention for minor planet provisional designations, the first letter represents the half-month of the year of discovery while the second letter and numbers indicate the order of discovery within that half-month. In the case for 2001 KX76, the first letter 'K' corresponds to the second half-month of May 2001 while the succeeding letter 'X' indicates that it is the 23rd object discovered on the 77th cycle of discoveries (with 76 cycles completed). Each cycle consists of 25 letters representing discoveries, hence 23 + (76 cycles × 25 letters) = 1,923.
  4. ^ The plutino classification is named after the dwarf planet Pluto, largest member of this group.
  5. ^ The current estimates of Pluto and Charon's diameters are 2376 km and 1212 km, respectively. One-third of Pluto's diameter is 792 km and three-fifths of Charon's diameter is 727 km—compare to Ixion's diameter of 710 km.

References

  1. ^ Brown, Michael (July 2005). "Icy planetoids of the outer solar system HST Proposal 10545". Mikulski Archive for Space Telescopes. Space Telescope Science Institute: 10545. Bibcode:2005hst..prop10545B. Retrieved 30 November 2019.
  2. ^ "JPL Small-Body Database Browser: 28978 Ixion (2001 KX76)" (2018-06-20 last obs.). Jet Propulsion Laboratory. 13 July 2019. Retrieved 7 April 2021.
  3. ^ "Ixion". Lexico UK English Dictionary. Oxford University Press. Archived from the original on February 24, 2020.
    "Ixion". Merriam-Webster.com Dictionary. Merriam-Webster.
  4. ^ Buie, M. W. "Orbit Fit and Astrometric record for 28978". Southwest Research Institute. Retrieved 26 April 2017.
  5. ^ "28978 Ixion (2001 KX76)". Minor Planet Center. International Astronomical Union. Retrieved 26 April 2017.
  6. ^ "Ixionian". Oxford English Dictionary (Online ed.). Oxford University Press. (Subscription or participating institution membership required.)
  7. ^ "Horizons Batch for 28978 Ixion on 2070-Sep-24" (Perihelion occurs when rdot flips from negative to positive). JPL Horizons. Retrieved 2023-08-27. (JPL#19/Soln.date: 2023-May-22)
  8. ^ "(28978) Ixion 2020 Oct 13". IOTA Asteroid Occultation Results Webpage. International Occultation Timing Association. 13 October 2020. Retrieved 24 October 2020.
  9. ^ Levine, Stephen E.; Zuluaga, Carlos A.; Person, Michael J.; Sickafoose, Amanda A.; Bosh, Amanda A.; Collins, Michael (April 2021). "Occultation of a Large Star by the Large Plutino (28978) Ixion on 2020 October 13 UTC". The Astronomical Journal. 161 (5): 210. Bibcode:2021AJ....161..210L. doi:10.3847/1538-3881/abe76d. S2CID 233545793.
  10. ^ Galiazzo, M.; de la Fuente Marcos, C.; de la Fuente Marcos, R.; Carraro, G.; Maris, M.; Montalto, M. (July 2016). "Photometry of Centaurs and trans-Neptunian objects: 2060 Chiron (1977 UB), 10199 Chariklo (1997 CU26), 38628 Huya (2000 EB173), 28978 Ixion (2001 KX76), and 90482 Orcus (2004 DW)". Astrophysics and Space Science. 361 (7): 15. arXiv:1605.08251. Bibcode:2016Ap&SS.361..212G. doi:10.1007/s10509-016-2801-5. ISSN 1572-946X. S2CID 119204060.
  11. ^ Rousselot, Philippe; Petit, J. (October 2010). Photometric Study Of 28978 Ixion At Small Phase Angle. 42nd DPS Meeting. American Astronomical Society. Bibcode:2010DPS....42.4019R. 40.19.
  12. ^ Verbiscer, Anne J.; Helfenstein, Paul; Porter, Simon B.; Benecchi, Susan D.; Kavelaars, J. J.; Lauer, Tod R.; et al. (April 2022). "The Diverse Shapes of Dwarf Planet and Large KBO Phase Curves Observed from New Horizons". The Planetary Science Journal. 3 (4): 31. Bibcode:2022PSJ.....3...95V. doi:10.3847/PSJ/ac63a6. 95.
  13. ^ Barucci, M. Antonietta; Brown, Michael E.; Emery, Joshua P.; Merlin, Frederic (2008). "Composition and Surface Properties of Transneptunian Objects and Centaurs" (PDF). The Solar System Beyond Neptune. University of Arizona Press. pp. 143–160. Bibcode:2008ssbn.book..143B. ISBN 978-0-8165-2755-7.
  14. ^ Fulchignoni, Marcello; Belskaya, Irina; Barucci, Maria Antonietta; De Sanctis, Maria Cristina; Doressoundiram, Alain (2008). "Transneptunian Object Taxonomy" (PDF). The Solar System Beyond Neptune. University of Arizona Press. pp. 181–192. Bibcode:2008ssbn.book..181F. ISBN 978-0-8165-2755-7.
  15. ^ Hainaut, O. R.; Boehnhardt, H.; Protopapa, S. (October 2012). "Colours of minor bodies in the outer solar system. II. A statistical analysis revisited" (PDF). Astronomy & Astrophysics. 546: 20. arXiv:1209.1896. Bibcode:2012A&A...546A.115H. doi:10.1051/0004-6361/201219566. S2CID 54776793.
  16. ^ "(28978) Ixion–Ephemerides". Asteroids Dynamic Site. Department of Mathematics, University of Pisa, Italy. Retrieved 26 April 2017.
  17. ^ Alvarez-Candal, A.; Pinilla-Alonso, N.; Ortiz, J. L.; Duffard, R.; Morales, N.; Santos-Sanz, P.; et al. (February 2016). "Absolute magnitudes and phase coefficients of trans-Neptunian objects" (PDF). Astronomy & Astrophysics. 586: 33. arXiv:1511.09401. Bibcode:2016A&A...586A.155A. doi:10.1051/0004-6361/201527161. S2CID 119219851. A155.
  18. ^ Tancredi, G.; Favre, S. (2008). "Which are the dwarfs in the solar system?" (PDF). Asteroids, Comets, Meteors. Retrieved 16 October 2019.
  19. ^ Brown, Michael E. (13 September 2019). "How many dwarf planets are there in the outer solar system?". California Institute of Technology. Retrieved 5 November 2019.
  20. ^ Grundy, W. M.; Noll, K. S.; Buie, M. W.; Benecchi, S. D.; Ragozzine, D.; Roe, H. G. (December 2018). "The Mutual Orbit, Mass, and Density of Transneptunian Binary Gǃkúnǁʼhòmdímà ((229762) 2007 UK126)" (PDF). Icarus. 334: 30–38. Bibcode:2019Icar..334...30G. doi:10.1016/j.icarus.2018.12.037. S2CID 126574999. Archived from the original on 7 April 2019.
  21. ^ "Kuiper Belt Object Found Possibly As Large As Pluto's Moon" (Press release). National Optical Astronomy Observatory. 2 July 2001. Retrieved 5 November 2019.
  22. ^ Buie, M. W. "The Deep Ecliptic Survey: Exploring the outer solar system in search of trans-Neptunian objects". Southwest Research Institute. Retrieved 9 November 2019.
  23. ^ Marsden, Brian G. (1 July 2001). "MPEC 2001-N01 : 2001 FT185, 2001 KW76, 2001 KX76, 2001 KY76, 2001 KZ76, 2001 KA77". Minor Planet Electronic Circular. Minor Planet Center.
  24. ^ Buie, M. W. "DES: Looker Statistics for the night of 010521". Southwest Research Institute. Retrieved 5 November 2019.
  25. ^ Zimmermann, Kim Ann (17 May 2017). "Scorpius Constellation: Facts About the Scorpion". Space.com. Retrieved 6 November 2019.
  26. ^ Whitehouse, David (3 July 2001). "Large world found near Pluto". BBC News. Archived from the original on 9 October 2002. Retrieved 6 November 2019.
  27. ^ "Virtual Telescope Observes Record-Breaking Asteroid". European Southern Observatory. 23 August 2001. Bibcode:2001eso..presP..27. Archived from the original on 7 October 2019. Retrieved 5 November 2019.
  28. ^ "New- And Old-Style Minor Planet Designations". Minor Planet Center. International Astronomical Union. Retrieved 6 November 2019.
  29. ^ Green, Daniel W. E. (5 July 2001). "IAUC 7657: 2001cz; 1993J, 1979C; 2001 KX_76". Central Bureau for Astronomical Telegrams. 7657. International Astronomical Union: 3. Bibcode:2001IAUC.7657....3M.
  30. ^ "M.P.S. 32834" (PDF). Minor Planet Center. International Astronomical Union. 19 August 2001. Retrieved 10 November 2019.
  31. ^ Marsden, Brian G. (11 August 2001). "MPEC 2001-P28 : 2001 KX76". Minor Planet Electronic Circular. 2001-P28. Minor Planet Center. Bibcode:2001MPEC....P...28G.
  32. ^ "M.P.C. 43346" (PDF). Minor Planet Center. International Astronomical Union. 2 September 2001. Retrieved 10 November 2019.
  33. ^ "How Are Minor Planets Named?". Minor Planet Center. International Astronomical Union. Retrieved 11 November 2019.
  34. ^ Graves, Robert (1955). "Ixion". The Greek Myths. Vol. 1. Penquin Books. ISBN 9780807600542. Retrieved 11 November 2019.
  35. ^ Schmadel, Lutz D. (2006). "(28978) Ixion". Dictionary of Minor Planet Names – (28978) Ixion, Addendum to Fifth Edition: 2003–2005. Springer Berlin Heidelberg. p. 1147. doi:10.1007/978-3-540-29925-7. ISBN 978-3-540-00238-3.
  36. ^ "M.P.C. 45236" (PDF). Minor Planet Center. International Astronomical Union. 28 March 2002. Retrieved 5 November 2019.
  37. ^ Miller, Kirk (26 October 2021). "Unicode request for dwarf-planet symbols" (PDF). unicode.org.
  38. ^ Licandro, J.; Ghinassi, F.; Testi, L. (June 2002). "Infrared spectroscopy of the largest known trans-Neptunian object 2001 KX76" (PDF). Astronomy & Astrophysics. 388: L9–L12. arXiv:astro-ph/0204104. Bibcode:2002A&A...388L...9L. doi:10.1051/0004-6361:20020533. S2CID 7577024.
  39. ^ Johnston, W. R. (13 July 2019). "List of Known Trans-Neptunian Objects". Johnston's Archive. Retrieved 5 November 2019.
  40. ^ Ortiz, J. L.; Gutiérrez, P. J.; Casanova, V.; Sota, A. (September 2003). "A study of short term rotational variability in TNOs and Centaurs from Sierra Nevada Observatory" (PDF). Astronomy & Astrophysics. 407 (3): 1149–1155. Bibcode:2003A&A...407.1149O. doi:10.1051/0004-6361:20030972. S2CID 55292212.
  41. ^ Boehnhardt, H.; Bagnulo, S.; Muinonen, K.; Barucci, M. A.; Kolokolova, L.; Dotto, E.; et al. (February 2004). "Surface characterization of 28978 Ixion (2001 KX76)" (PDF). Astronomy & Astrophysics. 415 (2): L21–L25. Bibcode:2004A&A...415L..21B. doi:10.1051/0004-6361:20040005.
  42. ^ Sheppard, Scott S.; Jewitt, David C. (June 2003). "Hawaii Kuiper Belt Variability Project: An Update" (PDF). Earth, Moon, and Planets. 92 (1–4): 207–219. arXiv:astro-ph/0309251. Bibcode:2003EM&P...92..207S. doi:10.1023/B:MOON.0000031943.12968.46. ISSN 1573-0794. S2CID 189905992.
  43. ^ Bertoldi, Frank (7 October 2002). "Beyond Pluto: Max-Planck radioastronomers measure the sizes of distant minor planets" (Press release). Argelander-Instituts für Astronomie. Retrieved 11 November 2019.
  44. ^ Altenhoff, W. J.; Bertoldi, F.; Menten, K. M. (February 2004). "Size estimates of some optically bright KBOs" (PDF). Astronomy & Astrophysics. 415 (2): 771–775. Bibcode:2004A&A...415..771A. doi:10.1051/0004-6361:20035603.
  45. ^ Grundy, W. M.; Knoll, K. S.; Stephens, D. C. (July 2005). "Diverse Albedos of Small Trans-Neptunian Objects". Icarus. 176 (1): 184–192. arXiv:astro-ph/0502229. Bibcode:2005Icar..176..184G. doi:10.1016/j.icarus.2005.01.007. S2CID 118866288.
  46. ^ Stansberry, J. A.; Cruikshank, D. P.; Grundy, W. G.; Margot, J. L.; Emery, J. P.; Fernández, Y. R.; Reike, G. H. (August 2005). Albedos, Diameters (and a Density) of Kuiper Belt and Centaur Objects. 37th DPS Meeting. Vol. 37. American Astronomical Society. p. 737. Bibcode:2005DPS....37.5205S. 52.05.
  47. ^ Cruikshank, D. P.; Barucci, M. A.; Emery, J. P.; Fernández, Y. R.; Grundy, W. M.; Noll, K. S.; Stansberry, J. A. (2005). "Physical Properties of Transneptunian Objects" (PDF). Protostars and Planets V. University of Arizona Press. pp. 879–893. ISBN 978-0-8165-2755-7.
  48. ^ Stansberry, John; Grundy, Will; Brown, Mike; Cruikshank, Dale; Spencer, John; Trilling, David; Margot, Jean-Luc (2008). "Physical Properties of Kuiper Belt and Centaur Objects: Constraints from the Spitzer Space Telescope" (PDF). The Solar System Beyond Neptune. University of Arizona Press. pp. 161–179. arXiv:astro-ph/0702538. Bibcode:2008ssbn.book..161S. ISBN 978-0-8165-2755-7.
  49. ^ Brown, Michael E. (2008). "The Largest Kuiper Belt Objects" (PDF). The Solar System Beyond Neptune. University of Arizona Press. pp. 335–344. Bibcode:2008ssbn.book..335B. ISBN 978-0-8165-2755-7.
  50. ^ Mommert, Michael (2013). Remnant Planetesimals and their Collisional Fragments (PDF). Refubium (Thesis). Freie Universität Berlin. doi:10.17169/refubium-6484. Retrieved 11 November 2019.
  51. ^ Lellouch, E.; Santos-Sanz, P.; Lacerda, P.; Mommert, M.; Duffard, R.; Ortiz, J. L.; et al. (September 2013). ""TNOs are Cool": A survey of the trans-Neptunian region. IX. Thermal properties of Kuiper belt objects and Centaurs from combined Herschel and Spitzer observations" (PDF). Astronomy & Astrophysics. 557: 19. arXiv:1202.3657. Bibcode:2013A&A...557A..60L. doi:10.1051/0004-6361/201322047.
  52. ^ Stern, S. A.; Grundy, W.; McKinnon, W. B.; Weaver, H. A.; Young, L. A.; Young, L. A.; et al. (September 2018). "The Pluto System After New Horizons". Annual Review of Astronomy and Astrophysics. 56: 357–392. arXiv:1712.05669. Bibcode:2018ARA&A..56..357S. doi:10.1146/annurev-astro-081817-051935. S2CID 119072504.
  53. ^ Buie, M. W.; Millis, R. L.; Wasserman, L. H.; Elliot, J. L.; Kern, S. D.; Clancy, K. B.; et al. (June 2003). "Procedures, Resources and Selected Results of the Deep Ecliptic Survey" (PDF). Earth, Moon, and Planets. 92 (1–4): 113–124. arXiv:astro-ph/0309251. Bibcode:2003EM&P...92..113B. doi:10.1023/B:MOON.0000031930.13823.be. ISSN 1573-0794. S2CID 14820512.
  54. ^ "List Of Trans-Neptunian Objects". Minor Planet Center. International Astronomical Union. Retrieved 25 November 2019.
  55. ^ Jewitt, David (June 2008). "The 1000 km Scale KBOs". Earth, Planetary, and Space Sciences. University of California, Los Angeles. Retrieved 27 September 2019.
  56. ^ Tancredi, Gonzalo (6 April 2010). "Physical and dynamical characteristics of icy "dwarf planets" (plutoids)". Proceedings of the International Astronomical Union. 5 (S263): 173–185. Bibcode:2010IAUS..263..173T. doi:10.1017/S1743921310001717.
  57. ^ Brown, Michael (July 2001). "A Search for Kuiper Belt Object Satellites HST Proposal 9110". Mikulski Archive for Space Telescopes. Space Telescope Science Institute: 9110. Bibcode:2001hst..prop.9110B. Retrieved 30 November 2019.
  58. ^ Marchi, S.; Lazzarin, M.; Magrin, S.; Barbieri, C. (September 2003). "Visible spectroscopy of the two largest known trans-Neptunian objects: Ixion and Quaoar" (PDF). Astronomy & Astrophysics. 408 (3): L17–L19. Bibcode:2003A&A...408L..17M. doi:10.1051/0004-6361:20031142.
  59. ^ Barkume, K. M.; Brown, M. E.; Schaller, E. L. (January 2008). "Near-Infrared Spectra of Centaurs and Kuiper Belt Objects". The Astronomical Journal. 135 (1): 55–67. Bibcode:2008AJ....135...55B. doi:10.1088/0004-6256/135/1/55.
  60. ^ DeMeo, F. E.; Fornasier, S.; Barucci, M. A.; Perna, D.; Protopapa, S.; Alvarez-Candal, A.; et al. (January 2009). "Visible and near-infrared colors of Transneptunian objects and Centaurs from the second ESO large program" (PDF). Astronomy & Astrophysics. 493 (1): 283–290. Bibcode:2009A&A...493..283D. doi:10.1051/0004-6361:200810561.
  61. ^ Lorin, O.; Rousselot, P. (April 2007). "Search for cometary activity in three Centaurs (60558) Echeclus, 2000 FZ53 and 2000 GM137 and two trans-Neptunian objects [(29981) 1999 TD10 and (28978) Ixion]" (PDF). Monthly Notices of the Royal Astronomical Society. 376 (2): 881–889. Bibcode:2007MNRAS.376..881L. doi:10.1111/j.1365-2966.2007.11487.x.
  62. ^ Gleaves, Ashley; Allen, Randall; Tupis, Adam; Quigley, John; Moon, Adam; Roe, Eric; Spencer, David; Youst, Nicholas; Lyne, James (13 August 2012). A Survey of Mission Opportunities to Trans-Neptunian Objects – Part II, Orbital Capture. AIAA/AAS Astrodynamics Specialist Conference. Minneapolis, Minnesota: American Institute of Aeronautics and Astronautics. doi:10.2514/6.2012-5066. ISBN 9781624101823.
  63. ^ Zangari, Amanda M.; Finley, Tiffany J.; Stern, S. Alan; Tapley, Mark B. (2018). "Return to the Kuiper Belt: Launch Opportunities from 2025 to 2040". Journal of Spacecraft and Rockets. 56 (3): 919–930. arXiv:1810.07811. Bibcode:2019JSpRo..56..919Z. doi:10.2514/1.A34329. S2CID 119033012.
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