Astronomy:38628 Huya

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Short description: Trans-Neptunian object
38628 Huya
Huya Hubble.png
Huya and its satellite, imaged by the Hubble Space Telescope on 6 May 2012
Discovery[1]
Discovered byIgnacio R. Ferrín et al.
Discovery siteLlano del Hato Obs.
Discovery date10 March 2000
Designations
(38628) Huya
Pronunciation/huːˈjɑː/ hoo-YAH
Named afterHuya
2000 EB173
Minor planet categoryTNO · plutino[2]
Kozai res.[3] · distant[4]
Orbital characteristics[1][2]
Epoch 17 December 2021 (JD 2459200.5)
Uncertainty parameter 1
Observation arc24.44 yr (8,926 days)
Earliest precovery date9 April 1996
|{{{apsis}}}|helion}}50.835 AU
|{{{apsis}}}|helion}}28.552 AU
39.694 AU
Eccentricity0.28068
Orbital period250.09 yr (91,345 d)
Mean anomaly8.038°
Mean motion0° 0m 14.188s / day
Inclination15.474°
Longitude of ascending node169.420°
|{{{apsis}}}|helion}}14 December 2014[5]
68.485°
Known satellites1
Physical characteristics
Mean diameter411.0±7.3 km (primary only)[6]
406±16 km (primary only)[7]
458±9.2 km (primary and secondary, estimate)[7][8]
Mass>5.01×1019 kg[lower-alpha 1]
Mean density>1.43 g/cm3[9][10]
≈0.8 g/cm3 (assuming hydrostatic equilibrium)[6]
Rotation period6.725±0.006 h[6]
5.28 h (fragmentary)[9]
4.45±0.07 h (fragmentary)[11]
6.75±0.01 h (fragmentary)[12]
Geometric albedo0.079±0.004 (primary only[6]
0.083±0.004 (primary and secondary)[7][6]
0.081±0.008[8]
IR (moderately red)[13][14]
B−V=0.96±0.01[15][16]
V−R=0.57±0.02[15]
V−I=1.2±0.02[15]
Apparent magnitude19.8 (opposition)[17]
19.11 (opposition,
R-band)[18]
Absolute magnitude (H)5.04±0.03[7]
5.048±0.021[19]
4.8 (assumed)[1][4]


38628 Huya (/huːˈjɑː/ hoo-YAH; provisional designation 2000 EB173) is a binary trans-Neptunian object located in the Kuiper belt, a region of icy objects orbiting beyond Neptune in the outer Solar System. Huya is classified as a plutino, a dynamical class of trans-Neptunian objects with orbits in a 3:2 orbital resonance with Neptune. It was discovered by the Quasar Equatorial Survey Team and was identified by Venezuelan astronomer Ignacio Ferrín in March 2000. It is named after Juyá, the mythological rain god of the Wayuu people native to South America.

Huya's surface is moderately red in color due to the presence of complex organic compounds on its surface. Water ice has been suspected to be also present on its surface, although water ice has not been directly detected on Huya. Huya is considered as a mid-sized trans-Neptunian object, with an estimated diameter of about 400 km (250 mi). Huya is considered to be a possible dwarf planet, though its relatively small size and dark surface may imply that it never collapsed into a solid body and was thus never in hydrostatic equilibrium.[20]

Huya has one known natural satellite, designated S/2012 (38628) 1. The satellite is relatively large compared to Huya and is expected to have slowed its rotation, although measurements of Huya's brightness variations have indicated that Huya's rotation may not be synchronous with the satellite's orbit.

History

Discovery

Huya was discovered on 10 March 2000 by a team of astronomers of the Quasar Equatorial Survey Team (QUEST), led by Gustavo Bruzual and Charles Baltay at the Llano del Hato National Astronomical Observatory in Mérida, Venezuela.[21][22] Huya was first identified by Venezuelan astronomer Ignacio Ferrín during a computer-assisted search through images taken from a six-hour survey of deep-sky objects including quasars and supernovae, using the Llano del Hato National Astronomical Observatory's 1-meter Schmidt telescope on the night of 15 March 2000.[23][22][24] At the time of discovery, Huya was located in the constellation of Virgo.[lower-alpha 2] The subtle movement of Huya was detected by the QUEST's computer program, which was designed to identify moving objects by superimposing multiple images.[22][21] The discovery team subsequently analyzed earlier images taken from previous QUEST surveys conducted during the same month in order to verify the orbital motion of Huya.[22]

The discovery of Huya was formally announced by the Minor Planet Center in a Minor Planet Electronic Circular on 3 June 2000.[23] It was given the provisional designation 2000 EB173 which indicates its year of discovery, with the first letter further specifying that the discovery took place in the first half of March.[26] The last letter and numbers of its designation indicate that Huya is the 4327th object discovered in the first half of March.[26] At that time, Huya was thought to be one of the largest minor planets in the Solar System due to its apparent magnitude of 20, which is relatively bright for a distant object.[22] This implied that it might be around one-fourth the size of Pluto and comparable in size to the dwarf planet Ceres.[21][24][27] Baltay, leader of the discovery team and chairman of Yale University's Department of Physics, proclaimed that the discovery was significant because it was the largest object discovered in the Kuiper belt since Pluto in 1930.[21] In an interview on their discovery, Baltay asserted:

The significance of this finding? It's just, Wow! After all these years, we can still find something new in our solar system. Some of it is luck. We looked in the right place. The other is the precision of our instrumentation.[24][21]

After the announcement of Huya's discovery, the discovery team found precovery images of Huya taken with the Palomar Observatory's Samuel Oschin telescope on 9 April 1996.[22][4] These precovery images of Huya from Palomar are the earliest known observations of Huya.[4][1] The precovery images along with subsequent follow-up observations in 2000 extended Huya's observation arc up to four years, which helped refine Huya's orbit.[22] By 2002, Huya was observed 303 times.[28] This was sufficient to accurately determine its orbit, so was assigned the minor planet number 38628 to Huya on 28 March 2002.[28][29]

Name

This minor planet is named after the mythological figure Huya (Juyá), the rain god of the Wayuu people indigenous to the Guajira Peninsula of northern Venezuela and Colombia.[30][31] In Wayuu mythology, Juyá is a hunter who controlled the rain and was married to Pulowi, the female figure related to the wind and dry seasons.[32] Juyá is also associated with the winter and lives in the celestial altitudes beyond the sun.[33] The discovery team led by Ferrín particularly chose the name to represent Venezuela's indigenous peoples that lived in the region where Huya was discovered.[31] Ferrín presumed that Huya had experienced multiple impact events during its formation, which he considered analogous to rain, a trait associated with Juyá.[31]

While searching for names, Ferrín and his team had agreed upon a naming scheme based on indigenous names with traits that are associated with the object's characteristics.[31] Among 20 potential names considered by Ferrín's team, they chose the name Juyá, altered to its equivalent phonetic English spelling Huya.[31] The name was later submitted and proposed to the International Astronomical Union (IAU), which then approved the name in 2003.[30] The Minor Planet Center published the naming citation on 1 May 2003.[30] Although the IAU's present naming convention for minor planets requires objects in the orbital class of plutinos (objects in 3:2 orbital resonance with Neptune) to be named after underworld deities,[29] these guidelines had not yet been established when Huya was named.[34]

Orbit

Polar view of Huya's orbit around the Sun, with the outer planets' orbits shown for comparison.

Huya is in a 2:3 mean-motion orbital resonance with Neptune, meaning that Huya completes two orbits around the Sun for every three orbits completed by Neptune.[35] Due to its 2:3 orbital resonance with Neptune, Huya is classified as a plutino, a dynamical class of objects with orbits similar to that of Pluto.[22] Huya orbits the Sun at an average distance of 39.8 astronomical unit|AU (5.95×109 km), taking 250 years to complete a full orbit.[1] Huya's orbit is inclined to the ecliptic by 15.5 degrees, slightly less than Pluto's orbital inclination of 17 degrees.[1][36] It has an elongated orbit with an orbital eccentricity of 0.28. Due to its eccentric orbit, its distance from the Sun varies over the course of its orbit, ranging from 28.5 AU at perihelion (closest distance) to 51.1 AU at aphelion (farthest distance).[1] Like Pluto, its resonance with Neptune prevents close approaches between Huya and the giant planets.[37] The minimum orbit intersection distance (MOID) between Huya and Neptune is 1.45 AU,[4] but due to the resonance, the two never come closer than 21 AU of each other.

Huya passed perihelion in December 2014,[5] and is now moving away from the Sun, approaching aphelion by 2139. (As of 2019), Huya is approximately 28.8 AU from the Sun, located in the direction of the constellation Ophiuchus.[38][39] Simulations by the Deep Ecliptic Survey (DES) show that Huya can acquire a perihelion distance (qmin) as small as 27.27 AU over the next 10 million years.[2]

The varying distances of Neptune, Pluto and Huya from the Sun, graphed over a period of one thousand years from 2007 to 3007
Distance between Huya and Neptune over the next 100,000 years. Due to the 2:3 resonance, Huya never comes closer than 21 AU of Neptune.
Huya's orbit, librating in a 2:3 resonance with Neptune, in a frame co-rotating with Neptune

Physical characteristics

Size

Size estimates for Huya
Year Diameter (km) Method Refs
2001 ~600 assumed albedo [22]
2003 <540 photometry [40]
2005 <548 thermal [41]
2005 480±50 thermal [42]
2007 546.5+47.8
−47.1
or 523.1+22.7
−21.9 		thermal
(Spitzer 2-Band) 		[43]
2007 532.6+24.4
−25.1 		thermal
(adopted) 		[43]
2012 438.7+26.5
−25.2 		thermal [44]
2012 384+98
−134 		photometry [45]
2013 438.5±0.5 best-fit albedo [46]
2013 458±9.2
or 406±16 (primary only) 		thermal [7]
2019 458+22
−21 		thermal [8]
2019 411.0±7.3 stellar occultation [6]
Artist's rendition of Huya and its satellite. Huya is unlikely to be spherical according to Grundy et al., who propose that dark, mid-sized TNOs such as Huya are unlikely to be in hydrostatic equilibrium.[20]

At the time of discovery, Huya was thought to be about one-fourth the size of Pluto, or 600 km (370 mi) in size, based on an initially measured bright absolute magnitude of 4.7 and an assumed dark albedo (reflectivity) of 0.04.[22] This initial size estimate of Huya made it one of the largest trans-Neptunian objects known at that time, ranking as the second-largest minor planet after Ceres.[lower-alpha 3][22][21][27] Subsequent measurements of Huya's thermal emission yielded higher albedo estimates for Huya, consequently corresponding to smaller diameter estimates.[47] Photometric and thermal observations of Huya in 2003 and 2005 placed an upper limit to Huya's diameter at 540–548 km (336–341 mi), based on a minimum albedo around 0.08.[40][41]

Early estimates for Huya's diameter were calculated from its apparently high absolute magnitude (brightness), was later discovered to be the combination of the brightnesses of the primary body (Huya) and its large satellite, whose existence was unknown until its discovery in 2012.[47][7][48] By subtracting the satellite's effects from Huya's brightness, astronomers were able to approximate Huya's true diameter.[7] Huya's mean diameter is estimated at 406 km (252 mi), based on measurements of Huya's thermal emission by the Herschel Space Observatory in 2013.[7] Compared to Pluto and its moon Charon, Huya is approximately one-sixth the diameter of Pluto and one-third the diameter of Charon.[lower-alpha 4]

On 18 March 2019, Huya occulted a bright 10.6-magnitude star, briefly dimming the star as Huya passed in front of it.[50][6][51] The stellar occultation was observed by astronomers across central Europe and Asia and was detected by 21 telescopes at 18 observation sites in the region.[6] Successful detections of the occultation yielded 14 chords from Romania, three chords from Turkey, and three chords from Israel.[6] Huya was shown to have an oblate shape, based on a best-fit elliptical model constructed from the chords obtained from the occultation, with a best fit projected ellipse of 435.2±7.0 by 388.2±12.2 km at the time of the occultation.[50][6] Assuming that Huya is a Maclaurin spheroid, it would be approximately 435 by 435 by 233 km in size, with a density of about 800 g/cm3.[6] No signs of a possible atmosphere or rings were detected during the occultation, with strong constraints put on the amount of debris in the vicinity of Huya.[50][6] Rings with a width smaller than 0.1 km, or an opacity of less than 50 percent, remain possible.[6]

Possible dwarf planet status

Huya was considered to be a possible dwarf planet due to its presumed high brightness, which corresponds to a large diameter.[47][52] Astronomer Gonzalo Tancredi considered Huya as a possible dwarf planet with an estimated diameter larger than 450 km (280 mi), the suggested minimum size for icy objects to maintain a spheroidal shape.[52][53] However, later measurements of Huya's diameter yielded smaller size estimates, casting doubt on this possibility.[47] Adopting Herschel's mean diameter estimate of 406 km (252 mi),[7] Huya is slightly larger than Saturn's moon Mimas, which is ellipsoidal in shape, and slightly smaller than Neptune's moon Proteus, which is irregular in shape.[lower-alpha 5] In 2019, William Grundy and colleagues proposed that trans-Neptunian objects in the size range of approximately 400–1,000 km (250–620 mi) are transitional between smaller, porous (and thus low-density) bodies and larger, denser, brighter and geologically differentiated planetary bodies such as dwarf planets.[20] Huya is situated at the lower end of the size range, implying that Huya's interior structure is likely highly porous and undifferentiated since its formation and thus is unlikely to be in hydrostatic equilibrium.[20] In a 2014 study, Audrey Thirouin and colleagues had suggested that the minimum density of Huya was 1.43 g/cm3, but this was a rough estimate derived indirectly from variations in brightness.[9] Based on a 2019 stellar occultation, Santos-Sanz et al. found a density of about 0.8 g/cm3 if Huya is a Maclaurin spheroid, and >0.859 g/cm3 if it is a Jacobi ellipsoid; however, the occultation found no evidence of an irregular shape for Huya, with their 2022 paper describing the plutino as being at least consistent with "a very round object".[6]

Spectra and surface

The reflectance spectrum of Huya appears moderately red and featureless in the infrared spectrum, lacking apparent absorption signatures of water ice and other volatile materials.[55][56][7] The scattered disc object 1996 TL66 shares a similarly featureless spectrum with Huya, though their visible colors differ.[57] Huya's featureless spectrum indicates that its surface is covered with a thick layer of dark organic compounds irradiated by solar radiation and cosmic rays.[57][58] Although water ice appears to be absent in Huya's infrared spectrum, some astronomers have detected subtle signs of water ice in its visible spectrum in 2011 and 2017.[14][59] The discrepancy of the presence of water ice between the visible and infrared spectra of Huya was interpreted as an indication of heterogeneity in Huya's surface composition.[7] Huya's surface is homogeneously covered with trace amounts of water ice, as subtle water ice absorption features recur in multiple observations of Huya's visible spectrum over the course of its rotation.[59] Early observations of Huya's spectrum in 2000 have identified a red spectral slope at wavelengths around 0.7 μm, typical of dark trans-Neptunian objects.[22] Additional near-infrared absorption features were also identified, and were attributed to the presence of aqueously altered silicate minerals on Huya's surface.[58][56]

The red color of Huya's surface results from the irradiation of organic compounds by solar radiation and cosmic rays, which produces dark, reddish tholins that cover its surface.[58] Huya's featureless spectrum indicates that its surface is covered with a thick layer of dark organic compounds irradiated by solar radiation and cosmic rays.[58] Compared to the large Kuiper belt object Varuna, which displays apparent signs of water ice, Huya's spectrum appears redder and featureless, suggesting that its surface is covered with a thick layer of tholins concealing water ice underneath.[58] It is thought that the layer of surface tholins on Huya is thicker than that of Varuna, as a result of a more intense radiation environment.[58] Best-fit models for these absorption features suggest that Huya's surface consists of a mixture of cometary ice tholins (ice tholin II),[60] nitrogen-rich Titan tholins,[61] as well as water ice.[56]

Spectrographic observations of Huya's spectrum with the Very Large Telescope in 2001 and 2002 have tentatively identified weak absorption features at near-infrared wavelengths around 0.6–0.82 μm, possibly indicating the presence of phyllosilicate materials on its surface.[56] The 0.6 μm absorption feature in Huya's spectrum resembles those in the spectra of stony S-type asteroids, which may suggest the presence of spinel group minerals, albeit in trace amounts as such minerals are unlikely to be abundant in trans-Neptunian objects.[56] Other absorption features near 0.7 μm in Huya's spectrum appear akin to those in the spectra of dark asteroids, indicating the presence of hydrous silicate minerals such as phyllosilicates, which may have been aqueously altered through heating induced by impact events or the radioactive decay of radionuclides in Huya's interior.[56] However, later observations of Huya's spectrum did not find any absorption features related to aqueously altered material, suggesting that they are likely concentrated in a small, localized area of Huya's surface.[59]

Brightness

Huya has a visual absolute magnitude (H) of 5.04 and a low geometric albedo of 0.083.[7] Its apparent magnitude, the brightness as seen from Earth, varies from 19.8 to 21.6 magnitudes.[17] Huya comes to opposition in June of each year at a visual apparent magnitude of 19.8.[17][62] At wavelengths of the R-band range, Huya appears brighter in red light,[22] with its R-band apparent magnitude reaching 19.11 magnitudes at opposition.[18] At the time of Huya's discovery, it was thought to be one of the brightest trans-Neptunian objects known, which corresponded to an initially large size estimate for Huya as it appeared relatively bright for a distant object.[22] As Huya comes to opposition, its brightness increases as a result of an opposition surge, in which its phase angle approaches zero. In 2001, long-term photometric observations of Huya were conducted to observe its opposition surge behavior and attempted to identify any indication of variability in Huya's brightness. The results showed a gradual increase in brightness near opposition, indicating a low geometric albedo. Huya became the first trans-Neptunian object other than Pluto to have its opposition surge measured.[18] Huya appeared to display very little variability in brightness, with an estimated light curve amplitude of less than 0.097 magnitudes.[18]

Rotation

The rotation period of Huya is unknown due to the flat appearance of its light curve, displaying very little variability in brightness.[63][64][65] Preliminary photometric observations of Huya in 2000 have reported no indication of variability greater than three percent of its brightness over a period of 1.25 hours.[63][22] Follow-up photometric observations of Huya at opposition in 2001 yielded a similarly flat light curve, with an estimated amplitude of less than 0.097 magnitudes.[18] The small amplitude of Huya's light curve suggests that it may be oriented in a pole-on configuration, with its rotational axis pointing toward Earth.[12] The discovery of a large satellite around Huya implies that it could be tidally locked to its satellite, although the satellite's orbit is unknown.[9] While Huya's rotation is expected to slow down on a timescale that is short compared to the age of the Solar System through mutual tidal forces with its satellite, several photometric observations of Huya indicate a variability of several hours, suggesting that Huya may not be tidally locked to its satellite.[12][9][11]

In 2002, Ortiz and colleagues obtained a fragmentary rotation period of 6.75±0.01 hours for Huya, along with other alternative periods of 6.68±0.01 and 6.82±0.01 hours.[12] Their inferred rotation period was derived from data sets of short-term photometry taken separately in February and March 2002.[12] Their mean solution of 6.75±0.01 for Huya's rotation period appeared consistent with previous photometric observations, with an amplitude less than 0.1 magnitudes.[12] However, the rotation period determined by Ortiz was later determined to be an alias of Huya's brightness variability.[9] In 2014, Thirouin suggested a shorter fragmentary rotation period of 5.28 hours, tentatively determined from short-term photometric observations conducted in 2010 through 2013.[9] Like the former rotation period inferred by Ortiz, the latter period obtained by Thirouin was based on fragmentary photometric data and may be erroneous by a factor of 30 percent or more.[1]

Exploration

In a study published by Ashley Gleaves and colleagues in 2012, Huya was considered as a potential target for an orbiter mission that would be launched on an Atlas V 551 or Delta IV HLV rocket. For an orbiter mission to Huya, the spacecraft would have a launch date in November 2027 and use a gravity assist from Jupiter, taking 20 to 25 years to arrive.[66] Gleaves concluded that Huya and Ixion were the most feasible targets for the orbiter, as the trajectories required the fewest maneuvers for orbital insertion around either.[66] For a flyby mission to Huya, planetary scientist Amanda Zangari calculated that a spacecraft could take just under 10 years to arrive at Huya using a Jupiter gravity assist, based on a launch date of 2027 or 2032. Huya would be approximately 31 to 37 AU from the Sun when the spacecraft arrives by 2040.[67] Alternative trajectories using gravity assists from Jupiter, Saturn, or Uranus have been also considered. A trajectory using gravity assists from Jupiter and Uranus could take at least 20 years, based a launch date of 2038 or 2039, whereas a trajectory using a gravity assist from Saturn could take over 16 years, based on a later launch date of 2040. Using these alternative trajectories for the spacecraft, Huya would be approximately 37 to 38 AU from the Sun when the spacecraft arrives before 2060.[67]

Satellite

S/2012 (38628) 1
38628-huya.gif
Hubble images of Huya and its satellite, taken one day apart between June and July 2002
Discovery[48]
Discovered byKeith S. Noll
William M. Grundy
Hilke Schlichting
Ruth Murray-Clay
Susan D. Benecchi
Discovery date6 May 2012
(announced on 12 July 2012)
Orbital characteristics[10]
~1740±80 km (projected distance)
Orbital period~3.2 d (assumed)
Satellite ofHuya
Physical characteristics[7]
Mean diameter213±30 km (assuming the same albedo as the primary)
Albedo0.083 (assumed)
Absolute magnitude (H)6.44


S/2012 (38628) 1 is the provisional designation for the only known satellite of Huya.[48][10] It was discovered by a team led by Keith Noll in Hubble Space Telescope observations obtained on 6 May 2012, and confirmed in reexamination of archival Hubble Space Telescope imagery from 30 June and 1 July 2002.[48] The discovery was reported to the International Astronomical Union and was announced on 12 July 2012.[48] Assuming the same albedo as Huya, the satellite is estimated to be about 213 km (132 mi) in diameter.[7] From Hubble images of Huya, the satellite's separation distance from the primary is estimated to be at least 1,740 km (1,080 mi).[10]

Characteristics

The satellite is 1.4 magnitudes dimmer than Huya (HV=5.04),[48] giving a visual absolute magnitude of 6.44 for the satellite.[7][lower-alpha 6] The satellite is relatively large compared to Huya, being slightly larger than half the primary's diameter of 406 km (252 mi).[10][7] The size ratio of the satellite to the primary is 0.525.[10] The large size ratio is analogous to the Pluto–Charon binary system, in which Pluto's large moon Charon is large and massive enough such that the center of mass (barycenter) is located in the space between Charon and Pluto.[49][9] The Huya system may be in a similar case, although no information about its barycenter is known.[9] With a large size compared to Huya, the satellite is expected to have slowed Huya's rotation such that both components become mutually tidally locked,[9] although several photometric observations of Huya indicate a rotation period of several hours, suggesting that Huya may not be tidally locked to its satellite.[12][11] If Huya is not tidally locked to its satellite, this implies that the satellite could have a very low density of around 0.5 g/cm3, which would result in a longer time for both components to become mutually tidally locked.[9]

The orbit of the satellite is poorly known due to the small number of resolved observations of Huya's satellite.[17] Consequently, a definitive mass and density estimate for Huya cannot be derived from the satellite's orbit.[7] Based on archival Hubble images of Huya taken in 2002, the satellite's angular separation distance from Huya is approximately 60 to 80 milliarcseconds,[48][17] corresponding to an approximate distance of 1740±80 km.[10] The orbital period of the satellite is estimated at about 3.2 days.[10]

Notes

  1. ↑ Calculated using the Herschel diameter estimate of 406 km (radius 203 km)[7] and presumed lower limit density of 1.43 g/cm3.[9] Assuming a spherical shape for Huya, the radius of 203 km yields a volume of approximately 3.504×107 km3. Multiplying the volume with its density of 1.43 g/cm3 yields an approximate mass of 5.011×1019 kg.
  2. ↑ The given equatorial coordinates of Huya during 10 March 2000 is  13h 20m 32.68s and −00° 09′ 06.6″,[23][4] which is close to the Virgo constellation's coordinates around  13h and 0°.[25]
  3. ↑ Pluto was still considered a planet at the time.
  4. ↑ The current estimates of Pluto and Charon's diameters are 2376 km and 1212 km, respectively.[49] One-sixth of Pluto's diameter is 396 km and one-third of Charon's diameter is 404 km, close to the 2013 Herschel estimate of 406±16 km for Huya's diameter.
  5. ↑ Mimas has a mean diameter of 396 km (246 mi) and Proteus has a mean diameter of 420 km (260 mi).[54] Adopting Herschel's mean diameter estimate of 406 km (252 mi) for Huya, it is larger than Mimas and smaller than Proteus.
  6. ↑ A larger magnitude value corresponds to a dimmer brightness.

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 "JPL Small-Body Database Browser: 38628 Huya (2000 EB173)". Jet Propulsion Laboratory. 13 July 2019. http://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2038628. 
  2. ↑ 2.0 2.1 2.2 Buie, M. W. (22 April 2007). "Orbit Fit and Astrometric record for 38628". Southwest Research Institute. http://www.boulder.swri.edu/~buie/kbo/astrom/38628.html. 
  3. ↑ Schwamb, Megan E.; Brown, Michael E.; Rabinowitz, David L.; Ragozzine, Darin (25 August 2010). "Properties of the Distant Kuiper Belt: Results from the Palomar Distant Solar System Survey". The Astrophysical Journal Letters 720 (2): 1691–1707. doi:10.1088/0004-637X/720/2/1691. Bibcode: 2010ApJ...720.1691S. 
  4. ↑ 4.0 4.1 4.2 4.3 4.4 4.5 "38628 Huya (2000 EB173)". Minor Planet Center. International Astronomical Union. http://www.minorplanetcenter.net/db_search/show_object?object_id=38628. 
  5. ↑ 5.0 5.1 "Horizons Batch for 38628 Huya on 2014-Dec-14". JPL Horizons. https://ssd.jpl.nasa.gov/api/horizons.api?format=text&COMMAND=%2738628%27&START_TIME=%272014-Dec-12%27&STOP_TIME=%272014-Dec-16%27&STEP_SIZE=%273%20hours%27&QUANTITIES=%2719%27. Retrieved 2023-08-27.  (JPL#42/Soln.date: 2023-Jul-28)
  6. ↑ 6.00 6.01 6.02 6.03 6.04 6.05 6.06 6.07 6.08 6.09 6.10 6.11 6.12 6.13 Santos-Sanz, Pablo et al. (24 May 2022). "Physical properties of the trans-Neptunian object (38628) Huya from a multi-chord stellar occultation". Astronomy & Astrophysics 664: A130. doi:10.1051/0004-6361/202141546. Bibcode: 2022A&A...664A.130S. https://www.aanda.org/articles/aa/pdf/forth/aa41546-21.pdf. 
  7. ↑ 7.00 7.01 7.02 7.03 7.04 7.05 7.06 7.07 7.08 7.09 7.10 7.11 7.12 7.13 7.14 7.15 7.16 7.17 Fornasier, S. et al. (July 2013). "TNOs are Cool: A survey of the trans-Neptunian region. VIII. Combined Herschel PACS and SPIRE observations of 9 bright targets at 70–500 μm". Astronomy & Astrophysics 555 (A15): 22. doi:10.1051/0004-6361/201321329. Bibcode: 2013A&A...555A..15F. https://www.aanda.org/articles/aa/full_html/2013/07/aa21329-13/aa21329-13.html. 
  8. ↑ 8.0 8.1 8.2 Lellouch, E.; Moreno, R.; Müller, T.; Fornasier, S.; Sanstos-Sanz, P.; Moullet, A.; Gurwell, M.; Stansberry, J. et al. (September 2019). "The thermal emission of Centaurs and Trans-Neptunian objects at millimeter wavelengths from ALMA observations". Monthly Notices of the Royal Astronomical Society 488 (3): 3035–3044. doi:10.1093/mnras/stz1880. 
  9. ↑ 9.00 9.01 9.02 9.03 9.04 9.05 9.06 9.07 9.08 9.09 9.10 9.11 Thirouin, A.; Knoll, K. S.; Ortiz, J. L.; Morales, N. (September 2014). "Rotational properties of the binary and non-binary populations in the Trans-Neptunian belt". Astronomy & Astrophysics 569 (A3): 20. doi:10.1051/0004-6361/201423567. Bibcode: 2014A&A...569A...3T. https://www.aanda.org/articles/aa/full_html/2014/09/aa23567-14/aa23567-14.html. 
  10. ↑ 10.0 10.1 10.2 10.3 10.4 10.5 10.6 10.7 Johnston, Wm. Robert (21 September 2014). "(38628) Huya". Johnston's Archive. http://www.johnstonsarchive.net/astro/astmoons/am-38628.html. 
  11. ↑ 11.0 11.1 11.2 Galiazzo, M.; de la Fuente Marcos, C.; de la Fuente Marcos, R.; Cararro, 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 (212). doi:10.1007/s10509-016-2801-5. ISSN 1572-946X. 
  12. ↑ 12.0 12.1 12.2 12.3 12.4 12.5 12.6 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". Astronomy & Astrophysics 407 (3): 1149–1155. doi:10.1051/0004-6361:20030972. Bibcode: 2003A&A...407.1149O. 
  13. ↑ Cruikshank, D. P.; Barucci, M. A.; Emery, J. P.; Fernández, Y. R.; Grundy, W. M.; Noll, K. S.; Stansberry, J. A. (2007). "Physical Properties of Transneptunian Objects". Protostars and Planets V. University of Arizona Press. pp. 879–893. ISBN 978-0-8165-2755-7. Bibcode: 2007prpl.conf..879C. https://www.lpi.usra.edu/books/PPV/8050.pdf. 
  14. ↑ 14.0 14.1 Barucci, M. A.; Alvarez-Candal, A.; Merlin, F.; Belskaya, I. N.; de Bergh, C.; Perna, D.; DeMeo, F.; Fornasier, S. (July 2011). "New insights on ices in Centaur and Transneptunian populations". Icarus 214 (1): 297–307. doi:10.1016/j.icarus.2011.04.019. Bibcode: 2011Icar..214..297B. https://pdfslide.net/documents/new-insights-on-ices-in-centaur-and-transneptunian-populations.html. 
  15. ↑ 15.0 15.1 15.2 Belskaya, Irina N.; Barucci, Maria A.; Fulchignoni, Marcello; Lazzarin, M. (April 2015). "Updated taxonomy of trans-neptunian objects and centaurs: Influence of albedo". Icarus 250: 482–491. doi:10.1016/j.icarus.2014.12.004. Bibcode: 2015Icar..250..482B. 
  16. ↑ "LCDB Data for (38628) Huya". Asteroid Lightcurve Database (LCDB). http://www.minorplanet.info/PHP/generateOneAsteroidInfo.php?AstInfo=38628. 
  17. ↑ 17.0 17.1 17.2 17.3 17.4 Grundy, Will (5 November 2019). "Huya (38628 2000 EB173)". Lowell Observatory. http://www2.lowell.edu/users/grundy/tnbs/38628_2000_EB173_Huya.html. 
  18. ↑ 18.0 18.1 18.2 18.3 18.4 Schaefer, Bradley E.; Rabinowitz, David L. (November 2002). "Photometric Light Curve for the Kuiper Belt Object 2000 EB173 on 78 Nights". Icarus 160 (1): 52–58. doi:10.1006/icar.2002.6958. 
  19. ↑ Rabinowitz, David L.; Schaefer, Bradley E.; Tourtellote, Suzanne W. (2007). "The Diverse Solar Phase Curves of Distant Icy Bodies. I. Photometric Observations of 18 Trans-Neptunian Objects, 7 Centaurs, and Nereid". The Astronomical Journal 133 (1): 26–43. doi:10.1086/508931. Bibcode: 2007AJ....133...26R. 
  20. ↑ 20.0 20.1 20.2 20.3 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)". Icarus. doi:10.1016/j.icarus.2018.12.037. http://www2.lowell.edu/~grundy/abstracts/2019.G-G.html. 
  21. ↑ 21.0 21.1 21.2 21.3 21.4 21.5 "Yale Astronomers Find New Minor Planet Between Neptune And Pluto". YaleNews (Yale University). 25 October 2000. https://news.yale.edu/2000/10/25/yale-astronomers-find-new-minor-planet-between-neptune-and-pluto. 
  22. ↑ 22.00 22.01 22.02 22.03 22.04 22.05 22.06 22.07 22.08 22.09 22.10 22.11 22.12 22.13 22.14 Ferrin, Ignacio et al. (16 February 2001). "Discovery of the Bright Trans-Neptunian Object 2000 EB173". The Astrophysical Journal Letters (American Astronomical Society) 548 (2). doi:10.1086/319109. 
  23. ↑ 23.0 23.1 23.2 "MPEC 2000-L09 : 2000 EB173". Minor Planet Center. International Astronomical Union. 3 June 2000. https://minorplanetcenter.net//iau/mpec/K00/K00L09.html. 
  24. ↑ 24.0 24.1 24.2 "Astronomers Find Large Asteroid Near Pluto". The New York Times. 26 October 2000. https://www.nytimes.com/2000/10/26/science/astronomers-find-large-asteroid-near-pluto.html. 
  25. ↑ Zimmermann, Kim Ann (13 July 2017). "Virgo Constellation: Facts about the Virgin". https://www.space.com/17021-virgo-constellation.html. 
  26. ↑ 26.0 26.1 "New- And Old-Style Minor Planet Designations". Minor Planet Center. International Astronomical Union. https://minorplanetcenter.net/iau/info/OldDesDoc.html. 
  27. ↑ 27.0 27.1 Chang, Kenneth (7 November 2000). "Studying Makeup of Miniplanets Beyond Pluto". The New York Times. https://www.nytimes.com/2000/10/26/science/astronomers-find-large-asteroid-near-pluto.html. 
  28. ↑ 28.0 28.1 "M.P.C. 45213". Minor Planet Center. International Astronomical Union. 28 March 2002. https://minorplanetcenter.net/iau/ECS/MPCArchive/2002/MPC_20020328.pdf. 
  29. ↑ 29.0 29.1 "How Are Minor Planets Named?". Minor Planet Center. International Astronomical Union. https://minorplanetcenter.net/iau/info/HowNamed.html. 
  30. ↑ 30.0 30.1 30.2 "M.P.C. 48397". Minor Planet Center. International Astronomical Union. 1 May 2003. https://minorplanetcenter.net/iau/ECS/MPCArchive/2003/MPC_20030501.pdf. 
  31. ↑ 31.0 31.1 31.2 31.3 31.4 Marquez, Humberto (30 August 2003). "Rain God Gets His Own Planet". Inter Press Service News Agency. http://www.ipsnews.net/interna.asp?idnews=19977. 
  32. ↑ Wilbert, Johannes; Simoneau, Karin; Perrin, Michael (1986). Folk Literature of the Guajiro Indians, Volume 2. 2. UCLA Latin American Center Publications. ISBN 9780879030636. https://books.google.com/books?id=VHtsAAAAMAAJ. Retrieved 18 October 2019. 
  33. ↑ Schmadel, Lutz D. (2006). "(38628) Huya". Dictionary of Minor Planet Names – (38628) Huya, Addendum to Fifth Edition: 2003–2005. Springer Berlin Heidelberg. p. 1178. doi:10.1007/978-3-540-29925-7. ISBN 978-3-540-00238-3. https://cds.cern.ch/record/1339660. 
  34. ↑ "How Are Minor Planets Named?". http://www.cfa.harvard.edu/iau/info/HowNamed.html. 
  35. ↑ "MPEC 2006-D28 : DISTANT MINOR PLANETS (2006 MAR. 26.0 TT)". Minor Planet Center. International Astronomical Union. 23 February 2006. https://minorplanetcenter.net//mpec/K06/K06D28.html. 
  36. ↑ Johnston, W. R. (13 July 2019). "List of Known Trans-Neptunian Objects". Johnston's Archive. http://www.johnstonsarchive.net/astro/tnoslist.html. 
  37. ↑ Malhotra, Renu; Arnett, Bill (20 September 1999). "Pluto's orbit". https://nineplanets.org/plutos-orbit/. 
  38. ↑ "(38628) Huya (observation prediction)". AstDyS. https://newton.spacedys.com/astdys/index.php?n=38628&pc=1.1.4.1&oc=500&y0=2021&m0=01&d0=01&h0=1&mi00. 
  39. ↑ "Huya position". 15 October 2019. http://www.sky-map.org/?ra=16.559893000000002&de=-6.890861000000001&zoom=9&show_grid=1&show_constellation_lines=1&show_constellation_boundaries=1&show_const_names=0&show_galaxies=1&show_box=1&box_ra=16.559893000000002&box_de=-6.890861&box_width=50&box_height=50&img_source=DSS2. 
  40. ↑ 40.0 40.1 Altenhoff, W. J.; Bertoldi, F.; Menten, K. M. (February 2004). "Size estimates of some optically bright KBOs". Astronomy & Astrophysics 415 (2): 771–775. doi:10.1051/0004-6361:20035603. Bibcode: 2004A&A...415..771A. https://astro.uni-bonn.de/~bertoldi/press/sedna/altenhoff_kbo.pdf. 
  41. ↑ 41.0 41.1 Grundy, W. M.; Knoll, K. S.; Stephens, D. C. (July 2005). "Diverse Albedos of Small Trans-Neptunian Objects". Icarus 176 (1): 184–192. doi:10.1016/j.icarus.2005.01.007. Bibcode: 2005Icar..176..184G. 
  42. ↑ 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. 37. American Astronomical Society. p. 737. 52.05. Bibcode: 2005DPS....37.5205S. 
  43. ↑ 43.0 43.1 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". The Solar System Beyond Neptune. University of Arizona Press. pp. 161–179. ISBN 978-0-8165-2755-7. https://www.lpi.usra.edu/books/ssbn2008/7017.pdf. 
  44. ↑ Mommert, M. et al. (May 2012). "TNOs are cool: A survey of the trans-Neptunian region V. Physical characterization of 18 Plutinos using Herschel-PACS observations". Astronomy & Astrophysics 541 (A93): 17. doi:10.1051/0004-6361/201118562. Bibcode: 2012A&A...541A..93M. 
  45. ↑ Sekiguchi, T.; Ootsubo, T.; Hasegawa, S.; Usui, F.; Cruikshank, D. P.; Dalle Ore, C. M.; Müller, T. G. (May 2012). "AKARI Observations of Minor Bodies in the Outer Solar System". Asteroids, Comets, Meteors. Lunar and Planetary Institute. 6477. Bibcode: 2012LPICo1667.6477S. https://www.lpi.usra.edu/meetings/acm2012/pdf/6477.pdf. 
  46. ↑ Mommert, Michael (2013). Remnant Planetesimals and their Collisional Fragments (PDF). Refubium (Thesis). Freie Universität Berlin. doi:10.17169/refubium-6484. Retrieved 24 October 2019.
  47. ↑ 47.0 47.1 47.2 47.3 Johnston, W. R. (23 October 2018). "TNO/Centaur diameters, albedos, and densities". Johnston's Archive. http://www.johnstonsarchive.net/astro/tnodiam.html. 
  48. ↑ 48.0 48.1 48.2 48.3 48.4 48.5 48.6 Green, Daniel W. E. (12 July 2012). "IAUC 9253: (38628) HUYA". Central Bureau for Astronomical Telegrams (International Astronomical Union) 9253. Bibcode: 2012IAUC.9253....2N. http://www.cbat.eps.harvard.edu/iauc/09200/09253.html#Item2. Retrieved 15 October 2019. 
  49. ↑ 49.0 49.1 Stern, S. A. et al. (September 2018). "The Pluto System After New Horizons". Annual Review of Astronomy and Astrophysics 56: 357–392. doi:10.1146/annurev-astro-081817-051935. Bibcode: 2018ARA&A..56..357S. 
  50. ↑ 50.0 50.1 50.2 Santos-Sanz, Pablo; Ortiz, J. L.; Popescu, M.; Sicardy, B.; Morales, N.; Benedetti-Rossi, G. (September 2019). "The multi-chord stellar occultation by the Transneptunian object (38628) Huya on March 18th 2019". EPSC-DPS Joint Meeting 2019. 13. European Planetary Science Congress. https://meetingorganizer.copernicus.org/EPSC-DPS2019/EPSC-DPS2019-666-5.pdf. 
  51. ↑ "Occultation by Huya (2019-03-18)". ERC Lucky Star project. 13 March 2019. http://lesia.obspm.fr/lucky-star/occ.php?p=15369. 
  52. ↑ 52.0 52.1 Tancredi, G.; Favre, S. (2008). "Which are the dwarfs in the solar system?". Asteroids, Comets, Meteors. http://www.lpi.usra.edu/meetings/acm2008/pdf/8261.pdf. 
  53. ↑ Tancredi, Gonzalo (6 April 2010). "Physical and dynamical characteristics of icy "dwarf planets" (plutoids)". Proceedings of the International Astronomical Union 5 (S263): 173–185. doi:10.1017/S1743921310001717. Bibcode: 2010IAUS..263..173T. 
  54. ↑ "Planetary Satellite Physical Parameters". Jet Propulsion Laboratory. 15 February 2019. http://ssd.jpl.nasa.gov/?sat_phys_par. 
  55. ↑ Jewitt, David C.; Luu, Jane X. (2001). "Colors and Spectra of Kuiper Belt Objects". The Astronomical Journal 122 (4): 2099–2114. doi:10.1086/323304. Bibcode: 2001AJ....122.2099J. https://cds.cern.ch/record/509438. 
  56. ↑ 56.0 56.1 56.2 56.3 56.4 56.5 de Bergh, C.; Boehnhardt, H.; Barucci, M. A.; Lazzarin, M.; Fornasier, S.; Romon-Martin, J.; Tozzi, G. P.; Doressoundiram, A. et al. (2004). "Aqueous altered silicates at the surface of two Plutinos?". Astronomy & Astrophysics 416 (2): 791–798. doi:10.1051/0004-6361:20031727. Bibcode: 2004A&A...416..791D. https://www.aanda.org/articles/aa/pdf/2004/11/aa3543.pdf. 
  57. ↑ 57.0 57.1 Brown, Michael E.; Blake, Geoffrey A.; Kessler, Jacqueline E. (October 2000). "Near-Infrared Spectroscopy of the Bright Kuiper Belt Object 2000 EB173". The Astrophysical Journal Letters 543 (2): L163–L165. doi:10.1086/317277. Bibcode: 2000ApJ...543L.163B. 
  58. ↑ 58.0 58.1 58.2 58.3 58.4 58.5 Licandro, J.; Oliva, E.; di Martino, M. (2001). "NICS-TNG infrared spectroscopy of trans-neptunian objects 2000 EB173 and 2000 WR106". Astronomy & Astrophysics 373 (3): 29–32L. doi:10.1051/0004-6361:20010758. Bibcode: 2001A&A...373L..29L. 
  59. ↑ 59.0 59.1 59.2 Merlin, F.; Hromakina, T.; Perna, D.; Hong, M. J.; Alvarez-Candal, A. (August 2017). "Taxonomy of trans-Neptunian objects and Centaurs as seen from spectroscopy". Astronomy & Astrophysics 604 (A86): 8. doi:10.1051/0004-6361/201730933. Bibcode: 2017A&A...604A..86M. 
  60. ↑ McDonald, Gene D.; Whited, Linda J.; DeRuiter, Cynthia; Khare, Bishun N.; Patnaik, Archita; Sagan, Carl (1996). "Production and Chemical Analysis of Cometary Ice Tholins". Icarus 122 (1): 107–117. doi:10.1006/icar.1996.0112. Bibcode: 1996Icar..122..107M. 
  61. ↑ McDonald, Gene D.; Thompson, W. Reid; Heinrich, Michael; Khare, Bishun N.; Sagan, Carl (1994). "Chemical Investigation of Titan and Triton Tholins". Icarus 108 (1): 137–145. doi:10.1006/icar.1994.1046. PMID 11539478. Bibcode: 1994Icar..108..137M. 
  62. ↑ "(38628) Huya–Ephemerides". Asteroids Dynamic Site. Department of Mathematics, University of Pisa, Italy. https://newton.spacedys.com/astdys2/index.php?pc=1.1.3.0&n=38628. 
  63. ↑ 63.0 63.1 Green, Daniel W. E. (20 July 2000). "IAUC 7459: C/1999 G5, C/1999 H7, C/1999 J12, C/1999 X2, C/2000 N2; 2000 EB_173; 2000cs". Central Bureau for Astronomical Telegrams (International Astronomical Union) 9253: 2. Bibcode: 2012IAUC.9253....2N. http://www.cbat.eps.harvard.edu/iauc/07400/07459.html. Retrieved 17 October 2019. 
  64. ↑ Sheppard, Scott S.; Jewitt, David C. (September 2002). "Time-resolved Photometry of Kuiper Belt Objects: Rotations, Shapes, and Phase Functions". The Astronomical Journal 124 (3): 1757–1775. doi:10.1086/341954. Bibcode: 2002AJ....124.1757S. http://www2.ess.ucla.edu/~jewitt/papers/LIGHTCURVES/SJ2002.pdf. 
  65. ↑ Sheppard, S. S.; Lacerda, P.; Ortiz, J. L. (2008). "Photometric Lightcurves of Transneptunian Objects and Centaurs: Rotations, Shapes, and Densities". in Barucci, A. M.. The Solar System Beyond Neptune. University of Arizona Press. pp. 129–142. ISBN 978-0-8165-2755-7. Bibcode: 2008ssbn.book..129S. http://web.gps.caltech.edu/~mbrown/out/kbbook/Chapters/Sheppard_Lightcurves.pdf. 
  66. ↑ 66.0 66.1 Gleaves, Ashley; Allen, Randall; Tupis, Adam; Quigley, John; Moon, Adam; Roe, Eric; Spencer, David; Youst, Nicholas et al. (13 August 2012) (in en-US). A Survey of Mission Opportunities to Trans-Neptunian Objects – Part II, Orbital Capture. Minneapolis, Minnesota: American Institute of Aeronautics and Astronautics. doi:10.2514/6.2012-5066. ISBN 9781624101823. http://trace.tennessee.edu/cgi/viewcontent.cgi?article=2518&context=utk_chanhonoproj. 
  67. ↑ 67.0 67.1 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. doi:10.2514/1.A34329. Bibcode: 2019JSpRo..56..919Z. 

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