38628 Huya

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. 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. At the time of discovery, Huya was located in the constellation of Virgo.{{efn|The given equatorial coordinates of Huya during 10 March 2000 is {{RA|13|20|32.68}} and {{Dec|-00|09|06.6}}, which is close to the Virgo constellation's coordinates around {{RA|13}} and {{Dec|0}}.}} The subtle movement of Huya was detected by the QUEST's computer program, which was designed to identify moving objects by superimposing multiple images. 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.

The discovery of Huya was announced by the Minor Planet Center in a Minor Planet Electronic Circular on 3 June 2000. It was given the provisional designation {{mp|2000 EB|173}} which indicates its year of discovery, with the first letter further specifying that the discovery took place in the first half of March. The last letter and numbers of its designation indicate that Huya is the 4327th object discovered in the first half of March. 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. Astronomers speculated that Huya could be the second-largest minor planet discovered after {{dp|Ceres}}, with a diameter around one-fourth the size of the then-planet Pluto. 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. In an interview on their discovery, Baltay asserted: {{blockquote|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.}}

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. These precovery images of Huya from Palomar are the earliest known observations of Huya. 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. By 2002, Huya was observed 303 times. This was sufficient to accurately determine its orbit, so was assigned the minor planet number 38628 to Huya on 28 March 2002.

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. 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. Juyá is also associated with the winter and lives in the celestial altitudes beyond the sun. 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. Ferrín presumed that Huya had experienced multiple impact events during its formation, which he considered analogous to rain, a trait associated with Juyá.

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. Among 20 potential names considered by Ferrín's team, they chose the name Juyá, altered to its equivalent phonetic English spelling Huya. The name was later submitted and proposed to the International Astronomical Union (IAU), which then approved the name in 2003. The Minor Planet Center published the naming citation on 1 May 2003. 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, these guidelines had not yet been established when Huya was named.

File:AnimatedOrbitOf38628Huya.gifs' orbits shown for comparison.]]

Huya is a trans-Neptunian object (TNO) 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. 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. Huya orbits the Sun at an average distance of {{convert|39.4|AU|e9km e9mi|lk=in|abbr=unit}}, taking 247 years to complete a full orbit.{{efn|name=barycentric|These orbital elements are expressed in terms of the Solar System Barycenter (SSB) as the frame of reference. Due to planetary perturbations, the Sun revolves around the SSB at non-negligible distances, so heliocentric-frame orbital elements and distances can vary in short timescales as shown in JPL-Horizons.}} Huya's orbit is inclined to the ecliptic by 15.5 degrees, slightly less than Pluto's orbital inclination of 17 degrees. 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 50.3 AU at aphelion (farthest distance). Like Pluto, Huya's orbital resonance prevents close approaches to Neptune. The minimum orbit intersection distance (MOID) between Huya and Neptune is approximately 1.4 AU, but due to the resonance, the two never come closer than 17 AU of each other.

Huya passed perihelion in December 2014, 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. Simulations by the Deep Ecliptic Survey (DES) show that Huya can acquire a perihelion distance (q_min) as small as 27.27 AU over the next 10 million years.

{{multiple image

|direction=horizontal

|align=center

|width1=355

|width2=323

|width3=200

|image1=HuyaDistancetoSunGraph.jpg

|image2=Huya-Neptune distance.png

|image3=Huya resonance.gif

|caption1=The varying distances of Neptune, Pluto and Huya from the Sun, graphed over a period of one thousand years from 2007 to 3007

|caption2=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.

|caption3=Huya's orbit, librating in a 2:3 resonance with Neptune, in a frame co-rotating with Neptune}}

File:Huya satellite occultations - Rommel et al. 2025 Fig 5.png (multicolored line) that spans the width of the body's silhouette.]]

The Huya system's current apparent magnitude, the brightness as seen from Earth, is about 20. Huya comes to opposition every June, when it appears brightest from Earth. As Huya's phase angle approaches zero during opposition, its brightness increases gradually, which indicates it has a low geometric albedo. Huya's low albedo has since been confirmed with measurements of Huya's diameter via thermal emission and occultation observations. Huya's brightness behavior at opposition, or opposition surge, was first studied in 2001; it is the first trans-Neptunian object other than Pluto to have its opposition surge studied. Huya appeared to display very little variability in brightness, with an estimated light curve amplitude of less than 0.097 magnitudes.

Stellar occultations by Huya occur when it passes in front of a star and blocks out its light, causing the star to dim for several seconds until Huya emerges. Observing stellar occultations by Huya can provide accurate measurements for its position, shape, and size.{{rp|page=1}}{{rp|page=1}} The first successful detection of a stellar occultation by Huya took place on 18 March 2019. The observing occultations for this occultation were favorable as the occulted star was bright (apparent magnitude 11) and the event was observable at central Europe and west Asia, where there were already many telescopes operated by amateur and professional astronomers.{{rp|page=3}} A total of 49 telescopes attempted to observe the occultation, with 21 positive detections reported from Romania, Turkey, and Israel.{{rp|page=3–4}} No signs of a possible atmosphere or rings were detected during the occultation, placing an upper limit surface atmospheric pressure of 10 nanobars, an upper limit ring opacity of 2.7%, and an upper limit ring width of {{cvt|0.1|km|mi}}.{{rp|page=9–10}} The satellite of Huya was not detected in the occultation.

Additional stellar occultations by the Huya system were observed on 28 March 2021, 17 February 2023, and 24 June 2023.{{rp|page=4}} In all three events, the satellite of Huya was detected, allowing for the determination of its orbit around Huya.{{rp|page=7}} Only one telescope detected the occultation in March 2021 and February 2023, whereas in June 2023 twelve out of the 30 participating telescopes detected the occultation.{{rp|page=7}} None of these occultation observations revealed any rings within {{cvt|9000|km|mi}} from Huya.{{rp|page=13}}

Results from the March 2019 and June 2023 occultations show that Huya has a flattened shape resembling an ellipse, with an equatorial diameter of {{cvt|436|km|mi}}.{{rp|page=8}} It is not known for certain whether Huya's true shape is an oblate spheroid or a triaxial ellipsoid; slight variations in Huya's shape between the 2019 and 2023 occultations could indicate rotation of a triaxial shape, although these could also be caused by measurement errors or topographic features on Huya.{{rp|page=8, 18}} Huya's brightness does not fluctuate enough to suggest a triaxial shape, which leads researchers to conclude that Huya's shape is more likely an oblate spheroid.{{rp|page=11}}{{rp|page=7}} If Huya has an oblate spheroid shape and its equator lies in the same plane as the orbit of its satellite, then Huya's polar diameter would be {{cvt|375|km|mi}}, about 14% shorter than its equatorial diameter.{{rp|page=8, 19}} These oblate spheroid dimensions correspond to a volume-equivalent diameter of {{cvt|415|km|mi}}.{{efn|name=volequiv|Volume-equivalent diameter of Huya calculated from $D\; =\; 2R\; =\; 2\backslash sqrt[3]\{abc\}$, where $a\; =\; b\; =\; 218.05\; \backslash pm\; 0.11\; km$ is Huya's equatorial radius and $c\; =\; 187.5\; \backslash pm\; 2.4\; km$ is Huya's polar radius.{{rp|page=8}} Uncertainty is calculated via error propagation.}} For comparison, Huya is about the size of Saturn's smallest round moon Mimas ({{cvt|396|km|mi|disp=or}}) and Neptune's largest non-spherical moon Proteus ({{cvt|416|km|mi|disp=or}}).

The diameter of Huya from occultations agrees with 2013 estimates of Huya's diameter from its infrared thermal emission.{{rp|page=2}} Before 2013, Huya was thought to be larger because its satellite was not known at the time; the satellite adds to Huya's overall brightness in visible light and infrared, thus making it seem brighter and larger than it actually is.{{rp|page=14}} Even earlier estimates of Huya's diameter proposed around the time of its discovery placed it at around {{convert|600|km|mi|abbr=on}}, or one-fourth the diameter of Pluto. These initial large diameter estimates led some astronomers to suspect Huya could be a dwarf planet candidate.{{rp|page=856}}

File:Huya system size comparison.png for scale]]

Since the orbit of Huya's satellite is known, the mass and density of Huya can be determined via Kepler's third law.{{rp|page=7}} The total mass of Huya and its satellite is {{val|4.5|e=19|u=kg}}.{{rp|page=13}} If Huya and its satellite both have spheroidal shapes with equal densities, then the bulk density of both objects in the Huya system is {{val|1.073|u=g/cm3}}.{{rp|page=8, 11}} If Huya has this density, then its mass is {{val|4.0|e=19|u=kg}}.{{efn|primarymass}} Comparing this density of the Huya system to other binary TNOs with known densities agrees with the observation that densities of TNOs are correlated with their diameter.{{rp|page=3}}

Huya's oblate shape, rotation period, and bulk density suggest that it is not in hydrostatic equilibrium. Assuming hydrostatic equilibrium for Huya predicts a low density of {{val|0.768|u=g/cm3}}, which in turn would predict an unrealistically high density for its satellite in order to keep the Huya system's total mass the same.{{rp|page=11}} Huya's lack of hydrostatic equilibrium is expected for its size, as the lower limit diameter for hydrostatic equilibrium in icy objects is estimated at around {{cvt|450|km|mi}}.{{rp|page=854}}{{rp|page=12}} At this size, Huya's icy interior is expected to be highly porous, having not experienced sufficient internal heating to undergo melting and differentiation.{{rp|page=31, 34}}

The surface of Huya appears dark and reddish in visible light, having a low visible geometric albedo of 0.079.{{rp|page=2}} In Barucci et al.'s four-class taxonomy scheme for TNO color indices, Huya falls under the IR group of TNOs with "moderately red" colors,{{rp|page=1294, 1296}} which is common among objects in the resonant and classical Kuiper belt populations.{{rp|page=305}} The dark, reddish color of Huya is caused by complex organic compounds (tholins) on its surface.{{rp|page=2}} Tholins are produced by the long-term irradiation of ices by solar radiation and cosmic rays,{{rp|page=2}} which chemically breaks them down and recombines them into more complex compounds.{{rp|page=7}} Tholins accumulate on Huya's surface over time, forming a thick layer that conceals fresh material like water ice underneath.{{rp|page=2}}

The surface composition of Huya can be studied via spectroscopy, particularly in near-infrared wavelengths where absorption signatures of various compounds like water ice and hydrocarbons can be found.{{rp|page=L163}}{{rp|page=L29}} Early attempts at studying Huya's near-infrared spectrum by ground-based telescopes were unable to detect any clear absorption features.{{rp|page=3, 7–8}} High-resolution near-infrared spectroscopy by the James Webb Space Telescope (JWST) in 2023 has revealed that Huya's surface contains various carbon-containing ices, including carbon monoxide (CO), carbon dioxide (CO₂) and its heavier isotopologue ¹³CO₂, methanol (CH₃OH), and other complex organic and aliphatic compounds.{{rp|page=3, 4}}{{rp|page=3, 4}} No clear signs of water ice were detected in Huya's near-infrared spectrum by JWST; while there is an absorption feature at 2.0 μm where water ice is expected (and was tentatively reported by ground-based spectroscopy),{{rp|page=3, 7–8}} it is more likely attributed to complex organics due to the absorption feature's different shape.{{rp|page=5}} Huya's near-infrared spectrum as seen by JWST is characterized by a prominent "double-dip" absorption feature at 3.0–3.7 μm, which has been spectroscopically identified in other TNOs by JWST.{{rp|page=5}} TNOs exhibiting this "double-dip" spectral feature are generally found on dynamically excited (high inclination and eccentricity) orbits, and are believed to have formed near the CO₂ ice line in the middle of the primordial Kuiper belt prior to Neptune's outward migration.{{rp|page=7}} Huya has been identified as an outlier among the "double-dip" TNOs due to its comparatively weaker CO₂ absorption features.{{rp|page=7}}

Visible spectroscopy of Huya by the Very Large Telescope in 2001 and 2002 has shown multiple weak absorption features at 0.5–0.9 μm, which has been interpreted as signs of aqueously-altered (hydrated) phyllosilicate minerals on Huya's surface.{{rp|page=795}}{{rp|page=3}} This finding is unexpected as TNOs are too cold for mineral hydration to occur. Nevertheless, it is possible that enough heat for mineral hydration could have been supplied in the past, through impact events or radioactive decay.{{rp|page=796–797}} However, later observations of Huya's visible spectrum in 2013 did not find any absorption features related to aqueously-altered silicate minerals, suggesting that they are either not real or are concentrated in a small, localized area of Huya's surface.{{rp|page=3, 6}}

The rotation period of Huya is difficult to measure photometrically with telescopes on Earth because it fluctuates very little in brightness as it rotates, due to its spheroidal shape.{{rp|page=2}} Several astronomers have attempted measuring Huya's rotation period via time series photometry, but were either unsuccessful due to insufficient precision or were able to tentatively identify rotation periods of a few hours. {{Asof|2025}}, astronomers believe Huya has a likely rotation period of 6.725 hours,{{rp|page=8}} based on photometry of observations from 2010–2013 and 2019.{{rp|page=5}} The light curve of Huya derived from these observations appears sinusoidal with a low amplitude of 0.031 magnitudes.{{rp|page=7}} The 6.725-hour rotation period of Huya is derived from this light curve by assuming it has a single-peaked periodicity due to a spheroidal shape.{{rp|page=9}} The axial tilt of Huya's rotation has not been measured, but it can be assumed to be aligned with the orbit of its satellite.{{rp|page=6}}

{{Main article|Satellite of 38628 Huya}}

File:Huya satellite HST 2002 annotated.gif in 2002]]

Huya has one known natural satellite, which has no official designation. Huya and its satellite form a binary system, and are together referred to as the Huya system.{{rp|page=2}} It was discovered by a team led by Keith Noll using Hubble Space Telescope images taken on 6 May 2012, and confirmed in reexamination of archival Hubble imagery from 2002. The satellite's discovery was announced by International Astronomical Union on 12 July 2012.

The satellite tightly orbits Huya with a separation distance of {{cvt|1900|km|mi}} and an orbital period of 3.46 days. It has a diameter between {{cvt|165–243|km|mi}}, or roughly half of Huya's diameter.{{rp|page=8}} With its large size relative to Huya, the satellite is expected to have tidally locked Huya's rotation, but observations of Huya's short rotation period show this is not the case.{{rp|page=7}} This suggests the satellite has a low density, estimated to be of around {{val|0.5|u=g/cm3}}. A similar scenario has been observed in the binary Kuiper belt object 174567 Varda, whose rotation is not tidally locked to its large satellite Ilmarë.{{rp|page=7}}

From the perspective of Earth, the opening angle of the Huya system's mutual orbit is slowly decreasing as Huya system moves along its orbit around the Sun. The Huya system will shift from a pole-on to an edge-on perspective by the year 2033, when the Huya system will enter mutual events season.{{rp|page=12}} During mutual events season, Huya and its satellite will take turns eclipsing and transiting each other, producing dips in brightness that last up to ~5 hours and have depths of up to ~0.25 magnitudes.{{rp|page=12}} Observations of these mutual events can help refine the Huya system's properties and can reveal the shapes, relative sizes, and surface albedo variations of Huya and its satellite.{{rp|page=12}}

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. Gleaves concluded that Huya and {{dp|Ixion}} 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 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. 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.

{{notelist|2|group=lower-alpha}}

{{clear}}

{{Reflist|30em|refs=

{{cite web

|type = 2019-05-01 last obs.

|title = JPL Small-Body Database Browser: 38628 Huya (2000 EB173)

|url = http://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2038628

|publisher = Jet Propulsion Laboratory

|date = 13 July 2019

|access-date = 20 February 2020}}

{{cite web

|title = JPL Horizons On-Line Ephemeris for 38628 (Huya) at epoch JD 2460000.5

|url = https://ssd.jpl.nasa.gov/horizons_batch.cgi?batch=1&COMMAND='38628'&TABLE_TYPE='ELEMENTS'&START_TIME='JD2460000.5'&STOP_TIME='JD2460200.5'&STEP_SIZE='1y'&CENTER='@0'&OUT_UNITS='AU-D'

|work = JPL Horizons On-Line Ephemeris System

|publisher = Jet Propulsion Laboratory

|accessdate = 18 January 2025}} Solution using the Solar System Barycenter. Ephemeris Type: Elements and Center: @0)

{{cite web

|title = JPL Horizons On-Line Ephemeris for 38628 Huya (2000 EB173) at epochs JD 2450000.5–2460000.5

|url = https://ssd.jpl.nasa.gov/horizons_batch.cgi?batch=1&COMMAND='38628'&TABLE_TYPE='ELEMENTS'&START_TIME='JD2450000.5'&STOP_TIME='JD2470000.5'&STEP_SIZE='200d'&CENTER='500@10'&OUT_UNITS='AU-D'

|work = JPL Horizons On-Line Ephemeris System

|publisher = Jet Propulsion Laboratory

|accessdate = 26 January 2025}} Solution using the Sun. Ephemeris Type: Elements and Center: @sun)

{{cite book

|title = Dictionary of Minor Planet Names – (38628) Huya, Addendum to Fifth Edition: 2003–2005

|first = Lutz D. |last = Schmadel

|publisher = Springer Berlin Heidelberg

|chapter = (38628) Huya

|page = 1178

|date = 2006

|isbn = 978-3-540-00238-3

|doi = 10.1007/978-3-540-29925-7|chapter-url = https://cds.cern.ch/record/1339660 }}

{{cite web

|title = 38628 Huya (2000 EB173)

|publisher = International Astronomical Union

|work = Minor Planet Center

|url = http://www.minorplanetcenter.net/db_search/show_object?object_id=38628

|access-date = 28 September 2017}}

{{cite web

|title = MPEC 2000-L09 : 2000 EB173

|publisher = International Astronomical Union

|work = Minor Planet Center

|url = https://minorplanetcenter.net//iau/mpec/K00/K00L09.html

|date = 3 June 2000

|access-date = 17 October 2019}}

{{cite web

|title = M.P.C. 45213

|publisher = International Astronomical Union

|work = Minor Planet Center

|url = https://minorplanetcenter.net/iau/ECS/MPCArchive/2002/MPC_20020328.pdf

|date = 28 March 2002

|access-date = 15 October 2019}}

{{cite web

|title = M.P.C. 48397

|publisher = International Astronomical Union

|work = Minor Planet Center

|url = https://minorplanetcenter.net/iau/ECS/MPCArchive/2003/MPC_20030501.pdf

|date = 1 May 2003

|access-date = 15 October 2019}}

{{cite web

|title = LCDB Data for (38628) Huya

|publisher = Asteroid Lightcurve Database (LCDB)

|url = http://www.minorplanet.info/PHP/generateOneAsteroidInfo.php?AstInfo=38628

|access-date = 28 September 2017}}

{{cite web

|title=(38628) Huya–Ephemerides

|work=Asteroids Dynamic Site

|publisher=Department of Mathematics, University of Pisa, Italy

|url=https://newton.spacedys.com/astdys2/index.php?pc=1.1.3.0&n=38628

|access-date=16 October 2019}}

{{cite web

|title=Horizons Batch for 38628 Huya on 2014-Dec-14

|publisher=JPL Horizons

|type=Perihelion occurs when rdot flips from negative to positive

|url=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

|access-date=2023-08-27}} (JPL#42/Soln.date: 2023-Jul-28)

{{cite journal

|title=Near-Infrared Spectroscopy of the Bright Kuiper Belt Object 2000 EB173

|first1=Michael E. |last1=Brown

|first2=Geoffrey A. |last2=Blake

|first3=Jacqueline E. |last3=Kessler

|date=October 2000

|journal=The Astrophysical Journal Letters

|volume=543

|number=2

|pages=L163–L165

|doi=10.1086/317277

|bibcode=2000ApJ...543L.163B|doi-access=free

}}

{{cite journal

|title=Discovery of the Bright Trans-Neptunian Object {{mp|2000 EB|173}}

|display-authors=etal

|first1=Ignacio |last1=Ferrin

|first2=D. |last2=Rabinowitz

|first3=B. |last3=Schaefer

|first4=J. |last4=Snyder

|first5=N. |last5=Ellman

|first6=B. |last6=Vicente

|journal=The Astrophysical Journal Letters

|publisher=American Astronomical Society

|volume=548

|issue=2

|date=16 February 2001

|doi-access=free

|doi=10.1086/319109

|arxiv=astro-ph/0011527

|s2cid=16937417}}

{{cite journal

|title=NICS-TNG infrared spectroscopy of trans-neptunian objects 2000 EB173 and 2000 WR106

|first1=J. |last1=Licandro

|first2=E. |last2=Oliva

|first3=M. |last3=di Martino

|date=2001

|journal=Astronomy & Astrophysics

|volume=373

|issue=3

|pages=29–32L

|doi=10.1051/0004-6361:20010758

|bibcode=2001A&A...373L..29L

|arxiv=astro-ph/0105434|s2cid=15690206 }}

{{cite journal

|title=Time-resolved Photometry of Kuiper Belt Objects: Rotations, Shapes, and Phase Functions

|url=http://www2.ess.ucla.edu/~jewitt/papers/LIGHTCURVES/SJ2002.pdf

|first1=Scott S. |last1=Sheppard

|first2=David C. |last2=Jewitt

|date=September 2002

|journal=The Astronomical Journal

|volume=124

|number=3

|pages=1757–1775

|doi=10.1086/341954

|arxiv=astro-ph/0205392

|bibcode=2002AJ....124.1757S|s2cid=55644670

}}

{{cite journal

|title=Photometric Light Curve for the Kuiper Belt Object {{mp|2000 EB|173}} on 78 Nights

|first1=Bradley E. |last1=Schaefer

|first2=David L. |last2=Rabinowitz

|date=November 2002

|journal=Icarus

|volume=160

|issue=1

|pages=52–58

|doi=10.1006/icar.2002.6958

|arxiv=astro-ph/0208261|s2cid=118935733 }}

{{cite journal

|title=A study of short term rotational variability in TNOs and Centaurs from Sierra Nevada Observatory

|first1=J. L. |last1=Ortiz

|first2=P. J. |last2=Gutiérrez

|first3=V. |last3=Casanova

|first4=A. |last4=Sota

|date=September 2003

|journal=Astronomy & Astrophysics

|volume=407

|number=3

|pages=1149–1155

|doi=10.1051/0004-6361:20030972

|bibcode=2003A&A...407.1149O|doi-access=free

}}

{{cite journal

|title=Size estimates of some optically bright KBOs

|url=https://astro.uni-bonn.de/~bertoldi/press/sedna/altenhoff_kbo.pdf

|first1=W. J. |last1=Altenhoff

|first2=F. |last2=Bertoldi

|first3=K. M. |last3=Menten

|date=February 2004

|journal=Astronomy & Astrophysics

|volume=415

|number=2

|pages=771–775

|doi=10.1051/0004-6361:20035603

|bibcode=2004A&A...415..771A}}

{{cite journal

|title=Diverse Albedos of Small Trans-Neptunian Objects

|first1=W. M. |last1=Grundy

|first2=K. S. |last2=Knoll

|first3=D. C. |last3=Stephens

|date=July 2005

|journal=Icarus

|volume=176

|issue=1

|pages=184–192

|doi=10.1016/j.icarus.2005.01.007

|arxiv=astro-ph/0502229

|bibcode=2005Icar..176..184G

|s2cid=118866288 }}

{{cite journal

|first1 = M. A. |last1 = Barucci

|first2 = I. |last2 = Belskaya

|first3 = M. |last3 = Fulchignoni

|first4 = M. |last4 = Birlan

|title = Taxonomy of Centaurs and Trans-Neptunian Objects

|journal = The Astronomical Journal

|date = September 2005

|volume = 130

|issue = 3

|pages = 1291–1298

|doi-access = free

|doi = 10.1086/431957

|bibcode = 2005AJ....130.1291B

|s2cid = 32008426}}

{{cite web

|first=M. W. |last=Buie

|date=22 April 2007

|title=Orbit Fit and Astrometric record for 38628

|url=http://www.boulder.swri.edu/~buie/kbo/astrom/38628.html

|publisher=Southwest Research Institute

|access-date=17 July 2008}}

{{cite journal

|title=Aqueous altered silicates at the surface of two Plutinos?

|first1=C. |last1=de Bergh

|first2=H. |last2=Boehnhardt

|first3=M. A. |last3=Barucci

|first4=M. |last4=Lazzarin

|first5=S. |last5=Fornasier

|first6=J. |last6=Romon-Martin

|first7=G. P. |last7=Tozzi

|first8=A. |last8=Doressoundiram

|first9=E. |last9=Dotto

|date=2004

|journal=Astronomy & Astrophysics

|volume=416

|number=2

|pages=791–798

|doi-access=free

|doi=10.1051/0004-6361:20031727

|bibcode=2004A&A...416..791D|hdl=11577/2443984

|hdl-access=free

}}

{{cite book

|title = Celestial Mechanics: The Waltz of the Planets

|first1 = Alessandra Celletti |last1 = Celletti

|first2 = Ettore |last2 = Perozzi

|publisher = Springer

|chapter = At the edge of the Solar System

|pages = 187–198

|date = 2007

|isbn = 978-0-387-68577-9

|doi = 10.1007/978-0-387-68577-9_10}}

{{cite journal

|display-authors=etal

|first1=M. A. |last1=Barucci

|first2=A. |last2=Alvarez-Candal

|first3=F. |last3=Merlin

|first4=I. N. |last4=Belskaya

|first5=C. |last5=de Bergh

|first6=D. |last6=Perna

|title=New insights on ices in Centaur and Transneptunian populations

|date=July 2011

|journal=Icarus

|volume=214

|issue=1

|pages=297–307

|doi=10.1016/j.icarus.2011.04.019

|bibcode=2011Icar..214..297B

|s2cid=120331897|url=https://hal.archives-ouvertes.fr/hal-00768794/file/PEER_stage2_10.1016%252Fj.icarus.2011.04.019.pdf }}

{{cite journal

|title=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

|url=https://www.aanda.org/articles/aa/full_html/2013/07/aa21329-13/aa21329-13.html

|display-authors=etal

|first1=S. |last1=Fornasier

|first2=E. |last2=Lellouch

|first3=T. |last3=Müller

|first4=P. |last4=Santos-Sanz

|first5=P. |last5=Panuzzo

|first6=C. |last6=Kiss

|journal=Astronomy & Astrophysics

|volume=555

|issue=A15

|pages=22

|date=July 2013

|doi=10.1051/0004-6361/201321329

|arxiv=1305.0449v2

|bibcode=2013A&A...555A..15F|s2cid=119261700

}}

{{cite book

|first1=John |last1=Stansberry

|first2=Will |last2=Grundy

|first3=Mike |last3=Brown

|first4=Dale |last4=Cruikshank

|first5=John |last5=Spencer

|first6=David |last6=Trilling

|first7=Jean-Luc |last7=Margot

|date=2008

|chapter-url=https://www.lpi.usra.edu/books/ssbn2008/7017.pdf

|chapter=Physical Properties of Kuiper Belt and Centaur Objects: Constraints from the Spitzer Space Telescope

|title=The Solar System Beyond Neptune

|pages=161–179

|publisher=University of Arizona Press

|isbn=978-0-8165-2755-7

|arxiv=astro-ph/0702538}}

{{cite journal

|first1 = Gonzalo |last1 = Tancredi

|first2 = Sofía |last2 = Favre

|title = Which are the dwarfs in the solar system?

|journal = Icarus

|date = June 2008

|volume = 195

|issue = 2

|pages = 851–862

|doi = 10.1016/j.icarus.2007.12.020

|bibcode = 2008Icar..195..851T

|s2cid = 120213376}}

{{cite conference

|title=AKARI Observations of Minor Bodies in the Outer Solar System

|url=https://www.lpi.usra.edu/meetings/acm2012/pdf/6477.pdf

|first1=T. |last1=Sekiguchi

|first2=T. |last2=Ootsubo

|first3=S. |last3=Hasegawa

|first4=F. |last4=Usui

|first5=D. P. |last5=Cruikshank

|first6=C. M. |last6=Dalle Ore|author6-link=Cristina Dalle Ore

|first7=T. G. |last7=Müller

|date=May 2012

|conference=Asteroids, Comets, Meteors

|publisher=Lunar and Planetary Institute

|issue=1667

|id=6477

|bibcode=2012LPICo1667.6477S}}

{{cite book

|title=A Survey of Mission Opportunities to Trans-Neptunian Objects – Part II, Orbital Capture

|url=http://trace.tennessee.edu/cgi/viewcontent.cgi?article=2518&context=utk_chanhonoproj

|first1=Ashley |last1=Gleaves

|first2=Randall

|first3=Adam |last3=Tupis |last2=Allen

|first4=John |last4=Quigley

|first5=Adam |last5=Moon

|first6=Eric |last6=Roe

|first7=David |last7=Spencer

|first8=Nicholas |last8=Youst

|first9=James |last9=Lyne

|location=Minneapolis, Minnesota

|language=en-US

|publisher=American Institute of Aeronautics and Astronautics

|date=13 August 2012

|doi=10.2514/6.2012-5066

|isbn=9781624101823}}

{{cite journal

|title=TNOs are cool: A survey of the trans-Neptunian region V. Physical characterization of 18 Plutinos using Herschel-PACS observations

|display-authors=etal

|first1=M. |last1=Mommert

|first2=A. W. |last2=Harris

|first3=C. |last3=Kiss

|first4=A. |last4=Pál

|first5=P. |last5=Santos-Sanz

|first6=J. |last6=Stansberry

|date=May 2012

|journal=Astronomy & Astrophysics

|volume=541

|issue=A93

|pages=17

|doi=10.1051/0004-6361/201118562

|arxiv=1202.3657

|bibcode=2012A&A...541A..93M|s2cid=119253817

}}

{{cite journal

|title=Rotational properties of the binary and non-binary populations in the Trans-Neptunian belt

|url=https://www.aanda.org/articles/aa/full_html/2014/09/aa23567-14/aa23567-14.html

|first1=A. |last1=Thirouin

|first2=K. S. |last2=Knoll

|first3=J. L. |last3=Ortiz

|first4=N. |last4=Morales

|date=September 2014

|journal=Astronomy & Astrophysics

|volume=569

|number=A3

|pages=20

|doi=10.1051/0004-6361/201423567

|arxiv=1407.1214|bibcode=2014A&A...569A...3T

|s2cid=119244456

}}

{{cite journal

|title=Updated taxonomy of trans-neptunian objects and centaurs: Influence of albedo

|first1=Irina N. |last1=Belskaya

|first2=Maria A. |last2=Barucci

|first3=Marcello |last3=Fulchignoni

|first4=M. |last4=Lazzarin

|date=April 2015

|journal=Icarus

|volume=250

|pages=482–491

|doi=10.1016/j.icarus.2014.12.004

|bibcode=2015Icar..250..482B}}

{{cite journal

|title=Taxonomy of trans-Neptunian objects and Centaurs as seen from spectroscopy

|first1=F. |last1=Merlin

|first2=T. |last2=Hromakina

|first3=D. |last3=Perna

|first4=M. J. |last4=Hong

|first5=A. |last5=Alvarez-Candal

|date=August 2017

|journal=Astronomy & Astrophysics

|volume=604

|number=A86

|pages=8

|doi=10.1051/0004-6361/201730933

|bibcode=2017A&A...604A..86M|doi-access=free

}}

{{cite journal

|title=Return to the Kuiper Belt: Launch Opportunities from 2025 to 2040

|first1=Amanda M. |last1=Zangari

|first2=Tiffany J. |last2=Finley

|first3=S. Alan |last3=Stern

|first4=Mark B. |last4=Tapley

|journal=Journal of Spacecraft and Rockets

|volume=56

|issue=3

|year=2018

|pages=919–930

|arxiv=1810.07811

|doi=10.2514/1.A34329|bibcode=2019JSpRo..56..919Z |s2cid=119033012 }}

{{cite journal

|display-authors = etal

|first1=E. |last1=Lellouch

|first2=R. |last2=Moreno

|first3=T. |last3=Müller

|first4=S. |last4=Fornasier

|first5=P. |last5=Sanstos-Sanz

|first6=A. |last6=Moullet

|title=The thermal emission of Centaurs and trans-Neptunian objects at millimeter wavelengths from ALMA observations

|date=December 2017

|journal=Astronomy & Astrophysics

|volume=608

|id=A45

|pages=21

|doi-access=free

|doi=10.1051/0004-6361/201731676

|arxiv=1709.06747

|bibcode=2017A&A...608A..45L}}

{{cite journal

|first1=W. M. |last1=Grundy

|first2=K. S. |last2=Noll

|first3=M. W. |last3=Buie

|first4=S. D. |last4=Benecchi

|first5=D. |last5=Ragozzine

|first6=H. G. |last6=Roe

|title=The Mutual Orbit, Mass, and Density of Transneptunian Binary Gǃkúnǁʼhòmdímà ({{mp|(229762) 2007 UK|126}})

|url=http://www2.lowell.edu/~grundy/abstracts/2019.G-G.html

|journal=Icarus

|doi=10.1016/j.icarus.2018.12.037

|date=December 2018

|bibcode=2019Icar..334...30G

|s2cid=126574999

|archive-url=https://web.archive.org/web/20190407045339/http://www2.lowell.edu/~grundy/abstracts/preprints/2019.G-G.pdf

|archive-date=7 April 2019}}

{{cite conference

|title=The multi-chord stellar occultation by the Transneptunian object (38628) Huya on March 18{{sup|th}} 2019

|url=https://meetingorganizer.copernicus.org/EPSC-DPS2019/EPSC-DPS2019-666-5.pdf

|display-authors=etal

|first1=Pablo |last1=Santos-Sanz

|first2=J. L. |last2=Ortiz

|first3=M. |last3=Popescu

|first4=B. |last4=Sicardy

|first5=N. |last5=Morales

|first6=G. |last6=Benedetti-Rossi

|date=September 2019

|conference=EPSC-DPS Joint Meeting 2019

|publisher=European Planetary Science Congress

|volume=13

|bibcode=2019EPSC...13..666S}}

{{cite journal

|title=Physical properties of the trans-Neptunian object (38628) Huya from a multi-chord stellar occultation

|display-authors=etal

|first1=Pablo |last1=Santos-Sanz

|first2=J. L. |last2=Ortiz

|first3=M. |last3=Popescu

|first4=B. |last4=Sicardy

|first5=N. |last5=Morales

|first6=G. |last6=Benedetti-Rossi

|date=24 May 2022

|arxiv=2205.12882

|journal=Astronomy & Astrophysics

|volume=664

|pages=A130

|doi-access=free

|doi=10.1051/0004-6361/202141546|bibcode=2022A&A...664A.130S

|s2cid=249063125

}}

{{cite journal

|title=IAUC 7459: C/1999 G5, C/1999 H7, C/1999 J12, C/1999 X2, C/2000 N2; 2000 EB_173; 2000cs

|volume=9253 |pages=2 |first=Daniel W. E. |last=Green

|publisher=International Astronomical Union

|journal=Central Bureau for Astronomical Telegrams

|date=20 July 2000

|url=http://www.cbat.eps.harvard.edu/iauc/07400/07459.html

|bibcode=2012IAUC.9253....2N

|access-date=17 October 2019}}

{{cite journal

|title=IAUC 9253: (38628) HUYA

|first=Daniel W. E. |last=Green

|publisher=International Astronomical Union

|journal=Central Bureau for Astronomical Telegrams

|date=12 July 2012

|volume=9253 |url=http://www.cbat.eps.harvard.edu/iauc/09200/09253.html#Item2

|url-status=dead

|archive-url=https://web.archive.org/web/20180510013226/http://lnfm1.sai.msu.ru/neb/rw/natsat/double/IAUC%209253.txt

|archive-date=10 May 2018

|bibcode=2012IAUC.9253....2N

|access-date=15 October 2019}}

{{cite news

|title=Yale Astronomers Find New Minor Planet Between Neptune And Pluto

|url=https://news.yale.edu/2000/10/25/yale-astronomers-find-new-minor-planet-between-neptune-and-pluto

|publisher=Yale University

|work=YaleNews

|date=25 October 2000

|access-date=16 October 2019}}

{{cite news

|title=Astronomers Find Large Asteroid Near Pluto

|url=https://www.nytimes.com/2000/10/26/science/astronomers-find-large-asteroid-near-pluto.html

|work=The New York Times

|date=26 October 2000

|access-date=16 October 2019}}

{{cite news

|title=Studying Makeup of Miniplanets Beyond Pluto

|url=https://www.nytimes.com/2000/10/26/science/astronomers-find-large-asteroid-near-pluto.html

|first=Kenneth |last=Chang

|work=The New York Times

|date=7 November 2000

|access-date=24 October 2019}}

{{cite web

|title=New- And Old-Style Minor Planet Designations

|url=https://minorplanetcenter.net/iau/info/OldDesDoc.html

|publisher=International Astronomical Union

|work=Minor Planet Center

|access-date=17 October 2019}}

{{cite web

|title=Virgo Constellation: Facts about the Virgin

|url=https://www.space.com/17021-virgo-constellation.html

|first=Kim Ann |last=Zimmermann

|website=Space.com

|date=13 July 2017

|access-date=17 October 2019}}

{{cite book

|title=Folk Literature of the Guajiro Indians, Volume 2

|url=https://books.google.com/books?id=VHtsAAAAMAAJ

|first1=Johannes |last1=Wilbert

|first2=Karin |last2=Simoneau

|first3=Michael |last3=Perrin

|publisher=UCLA Latin American Center Publications

|via=University of California, Los Angeles

|volume=2

|isbn=9780879030636

|year=1986

|access-date=18 October 2019}}

{{cite news

|title=Rain God Gets His Own Planet

|url=http://www.ipsnews.net/interna.asp?idnews=19977

|first=Humberto |last=Marquez

|publisher=Inter Press Service News Agency

|date=30 August 2003

|url-status=dead

|archive-url=https://web.archive.org/web/20030909233226/http://ipsnews.net/interna.asp?idnews=19977

|archive-date=9 September 2003

|access-date=18 October 2019}}

{{cite web

|title=How Are Minor Planets Named?

|url=https://minorplanetcenter.net/iau/info/HowNamed.html

|publisher=International Astronomical Union

|work=Minor Planet Center

|access-date=18 October 2019}}

{{Cite web |url=http://www.cfa.harvard.edu/iau/info/HowNamed.html |title=How Are Minor Planets Named? |access-date=18 October 2019 |archive-url=https://web.archive.org/web/20060701013613/http://www.cfa.harvard.edu/iau/info/HowNamed.html |archive-date=1 July 2006 |url-status=dead }}

{{cite web

|title=Huya (38628 2000 EB173)

|url=http://www2.lowell.edu/users/grundy/tnbs/38628_2000_EB173_Huya.html

|first=Will |last=Grundy

|publisher=Lowell Observatory

|date=5 November 2019

|access-date=22 October 2019}}

{{cite web

|title=Planetary Satellite Physical Parameters

|url=http://ssd.jpl.nasa.gov/?sat_phys_par

|publisher=Jet Propulsion Laboratory

|date=15 February 2019

|access-date=25 October 2019}}

{{cite web

|title=(38628) Huya (observation prediction)

|url=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

|publisher=AstDyS

|access-date=4 April 2021}}

{{cite web

|title = List of Known Trans-Neptunian Objects

|url = http://www.johnstonsarchive.net/astro/tnoslist.html

|work = Johnston's Archive

|first=W. R. |last=Johnston

|date = 13 July 2019

|access-date = 11 November 2019}}

{{cite web

|title=Huya position

|url=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

|website=sky-map.org

|date=15 October 2019

|access-date=27 October 2019}}

{{cite web

|title=Pluto's orbit

|url=https://nineplanets.org/plutos-orbit/

|first1=Renu |last1=Malhotra

|first2=Bill |last2=Arnett

|date=20 September 1999

|access-date=27 October 2019}}

{{cite journal

|title=Properties of the Distant Kuiper Belt: Results from the Palomar Distant Solar System Survey

|first1=Megan E. |last1=Schwamb

|first2=Michael E. |last2=Brown

|first3=David L. |last3=Rabinowitz

|first4=Darin |last4=Ragozzine

|date=25 August 2010

|journal=The Astrophysical Journal Letters

|volume=720

|issue=2

|pages=1691–1707

|doi-access=free

|doi=10.1088/0004-637X/720/2/1691

|arxiv=1007.2954

|bibcode=2010ApJ...720.1691S|s2cid=5853566 }}

{{cite journal

|display-authors=etal

|first1=A. C. |last1=Souza-Feliciano

|first2=B. J. |last2=Holler

|first3=N. |last3=Pinilla-Alonso

|first4=M. |last4=De Prá

|first5=R. |last5=Brunetto

|first6=T. |last6=Müller

|title=Spectroscopy of the binary TNO Mors-Somnus with the JWST and its relationship to the cold classical and plutino subpopulations observed in the DiSCo-TNO project

|journal=Astronomy & Astrophysics

|date=January 2024

|volume=681

|id=L17

|pages=8

|doi-access=free

|doi=10.1051/0004-6361/202348222

|bibcode=2024A&A...681L..17S

|s2cid=267154656}}

{{cite journal

|display-authors=etal

|first1=Noemí |last1=Pinilla-Alonso

|first2=Rosario |last2=Brunetto

|first3=Mário N. |last3=De Prá

|first4=Bryan J. |last4=Holler

|first5=Elsa |last5=Hénault

|first6=Ana Carolina de Souza |last6=Feliciano

|title=A JWST/DiSCo-TNOs portrait of the primordial Solar System through its trans-Neptunian objects

|journal=Nature Astronomy

|date=December 2024

|volume=9 |issue=2 |pages=230–244

|doi=10.1038/s41550-024-02433-2

|bibcode=2025NatAs...9..230P

|s2cid=274932942}}

{{cite journal

|display-authors=etal

|first1=F. L. |last1=Rommel

|first2=E. |last2=Fernández-Valenzuela

|first3=B. C. N. |last3=Proudfoot

|first4=J. L. |last4=Ortiz

|first5=B. E. |last5=Morgado

|first6=B. |last6=Sicardy

|title=Stellar occultation observations of (38628) Huya and its satellite: a detailed look into the system

|journal=The Planetary Science Journal

|date=February 2025

|volume=6

|issue=2

|id=48

|pages=21

|arxiv=2501.09739

|doi-access=free

|doi=10.3847/PSJ/adabc1

|bibcode=2025PSJ.....6...48R

|s2cid=275570412}}

}}

• [https://www.iota-es.de/JOA/JOA2021_2.pdf Beyond Jupiter: The World of Distant Minor Planets – (38628) Huya]
• [https://pdssbn.astro.umd.edu/data_other/HST_04_OUTER/38628%20.shtml Object: 38628 Huya (2000 EB173)] {{Webarchive|url=https://web.archive.org/web/20151022234236/http://pdssbn.astro.umd.edu/data_other/HST_04_OUTER/38628%20.shtml |date=2015-10-22 }} (Raw Hubble images of Huya)
• [https://web.archive.org/web/20080415042237/http://www.space.com/scienceastronomy/solarsystem/plutino_001024.html Planet 10? Tiny 'Plutino' Almost Qualifies]
• [http://news.bbc.co.uk/2/hi/science/nature/990041.stm 'Mini-Pluto' spotted orbiting the Sun]
• {{JPL small body}}

{{Minor planets navigator | |number=38628 | }}

{{Solar System moons (compact)}}

{{Trans-Neptunian objects}}

{{Small Solar System bodies}}

{{Solar System}}

{{Authority control}}

{{DEFAULTSORT:Huya}}

Category:38628 Huya

038628

Category:Binary trans-Neptunian objects

Category:Discoveries by Ignacio Ramón Ferrín Vázquez

Category:Named minor planets

038628

20000310

Category:Solar System