View source for Astronomy:38628 Huya

{{Short description|Trans-Neptunian object}}
{{Infobox planet
 | minorplanet     = yes
 | name            = 38628 Huya
 | background      = #C2E0FF
 | image           = File:Huya Hubble.png
 | image_scale      =
 | caption         = Huya and its satellite, imaged by the [[Astronomy:Hubble Space Telescope|Hubble Space Telescope]] on 6 May 2012
 | discovery_ref   = <ref name="jpldata"/>
 | discoverer      = Ignacio R. Ferrín et al.
 | discovery_site  = Llano del Hato Obs.
 | discovered      = 10 March 2000
 | earliest_precovery_date = 9 April 1996
 | mpc_name        = (38628) Huya
 | alt_names       = {{mp|2000 EB|173}}
 | pronounced      = {{IPAc-en|h|uː|ˈ|j|ɑː}} {{respell|hoo|YAH|'}}
 | named_after     = Huya
 | mp_category     = [[Astronomy:Trans-Neptunian object|TNO]]{{·}}[[Astronomy:Plutino|plutino]]<ref name="Buie"/><br/>[[Astronomy:Kozai mechanism|Kozai res.]]<ref name="Schwamb2010"/>{{·}}[[Astronomy:Distant minor planet|distant]]<ref name="MPC-object"/>
 | orbit_ref       = <ref name="jpldata"/><ref name="Buie"/>
 | epoch           = 17 December 2021 ([[Astronomy:Julian day|JD]] 2459200.5)
 | uncertainty     = 1
 | observation_arc = 24.44 yr (8,926 days)
 | aphelion        = 50.835 [[Astronomy:Astronomical unit|AU]]
 | perihelion      = 28.552 AU
 | time_periastron = 14 December 2014<ref name="Horizons2014"/>
 | semimajor       = 39.694 AU
 | eccentricity    = 0.28068
 | period          = 250.09 [[Astronomy:Julian year|yr]] (91,345 [[Astronomy:Julian year|d]])
 | mean_anomaly    = 8.038[[Degree (angle)|°]]
 | mean_motion     = {{Deg2DMS|0.0039411135|sup=ms}} / day
 | inclination     = 15.474°
 | asc_node        = 169.420°
 | arg_peri        = 68.485°
 | satellites      = 1
 | mean_diameter   = {{val|411.0|7.3|u=km}}  {{small|(primary only)}}<ref name="Santos-Sanz-2022"/><br/>{{val|406|16|u=km}} {{small|(primary only)}}<ref name="TNOsCool8"/><br/>{{val|458|9.2|u=km}} {{small|(primary and secondary, estimate)}}<ref name="TNOsCool8"/><ref name="Lellouch2019"/>
 | mass            = {{val|5.01|e=19|u=kg|p=>}}{{efn|Calculated using the Herschel diameter estimate of 406&nbsp;km (radius 203&nbsp;km)<ref name="TNOsCool8"/> and presumed lower limit density of {{val|1.43|u=g/cm3}}.<ref name="Thirouin2014"/> Assuming a spherical shape for Huya, the radius of 203&nbsp;km yields a volume of approximately {{val|3.504|e=7|u=km3}}. Multiplying the volume with its density of {{val|1.43|u=g/cm3}} yields an approximate mass of {{val|5.011|e=19|u=kg}}.}}
 | density         = {{val|1.43|u=g/cm3|p=>}}<ref name="Thirouin2014"/><ref name="johnston"/><br/>{{val|0.8|u=g/cm3|p=≈}} {{small|(assuming hydrostatic equilibrium)}}<ref name="Santos-Sanz-2022"/>
 | surface_grav    =
 | escape_velocity =
 | rotation        = {{val|6.725|0.006}} [[Hour|h]]<ref name="Santos-Sanz-2022"/><br/>{{val|5.28}} h {{small|(fragmentary)}}<ref name="Thirouin2014"/><br/>{{val|4.45|0.07}} h {{small|(fragmentary)}}<ref name="Galiazzo2016"/><br/>{{val|6.75|0.01}} h {{small|(fragmentary)}}<ref name="Ortiz2003"/>
 | spectral_type   = [[Astronomy:Trans-Neptunian object#Colors|IR]] (moderately red)<ref name="Cruikshank2007"/><ref name="Barucci2011"/><br/>B−V={{val|0.96|0.01}}<ref name="Belskaya2015"/><ref name="lcdb"/><br/>V−R={{val|0.57|0.02}}<ref name="Belskaya2015"/><br/>V−I={{val|1.2|0.02}}<ref name="Belskaya2015"/>
 | magnitude       = 19.8 ([[Astronomy:Opposition (planets)|opposition]])<ref name="Grundy-orbits"/><br/>19.11 (opposition,<br/>[[Astronomy:Photometric system|R-band]])<ref name="Schaefer2002"/>
 | abs_magnitude   = {{val|5.04|0.03}}<ref name="TNOsCool8"/><br/>{{val|5.048|0.021}}<ref name="Rabinowitz2006"/><br/>4.8 (assumed)<ref name="jpldata"/><ref name="MPC-object"/>
 | albedo          = {{val|0.079|0.004}} {{small|(primary only}}<ref name="Santos-Sanz-2022"/><br/>{{val|0.083|0.004}} {{small|(primary and secondary)}}<ref name="TNOsCool8"/><ref name="Santos-Sanz-2022"/><br/>{{val|0.081|0.008}}<ref name="Lellouch2019"/>
}}

'''38628 Huya''' ({{IPAc-en|h|uː|ˈ|j|ɑː}} {{respell|hoo|YAH|'}}; provisional designation '''{{mp|2000 EB|173}}''') is a [[Astronomy:Minor-planet moon|binary]] [[Astronomy:Trans-Neptunian object|trans-Neptunian object]] located in the [[Astronomy:Kuiper belt|Kuiper belt]], a region of icy objects orbiting beyond [[Astronomy:Neptune|Neptune]] in the outer [[Astronomy:Solar System|Solar System]]. Huya is classified as a [[Astronomy:Plutino|plutino]], a dynamical class of trans-Neptunian objects with orbits in a 3:2 orbital resonance with Neptune. It was discovered by the [[Astronomy:Quasar Equatorial Survey Team|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 [[Earth:South America|South America]].

Huya's surface is [[Astronomy:Trans-Neptunian object#Colors|moderately red]] in color due to the presence of complex [[Chemistry:Organic compound|organic compound]]s on its surface. Water [[Earth:Ice|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 {{convert|400|km|mi|abbr=on}}. Huya is considered to be a [[Astronomy:List of possible dwarf planets|possible]] [[Astronomy:Dwarf planet|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.<ref name="Grundy2019"/>

Huya has one known [[Astronomy:Natural satellite|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 [[Astronomy:Quasar Equatorial Survey Team|Quasar Equatorial Survey Team]] (QUEST), led by Gustavo Bruzual and Charles Baltay at the Llano del Hato National Astronomical Observatory in Mérida, Venezuela.<ref name="YaleNews"/><ref name="Ferrin2001"/> Huya was first identified by Venezuelan astronomer Ignacio Ferrín during a computer-assisted search through images taken from a six-hour survey of [[Astronomy:Deep-sky object|deep-sky object]]s including [[Astronomy:Quasar|quasar]]s and supernovae, using the Llano del Hato National Astronomical Observatory's 1-meter Schmidt telescope on the night of 15 March 2000.<ref name="MPEC-2000-L09"/><ref name="Ferrin2001"/><ref name="NYT-20001026"/> At the time of discovery, Huya was located in the [[Astronomy:Constellation|constellation]] of [[Astronomy:Virgo (constellation)|Virgo]].{{efn|The given [[Astronomy:Equatorial coordinate system|equatorial coordinate]]s of Huya during 10 March 2000 is {{RA|13|20|32.68}} and {{Dec|-00|09|06.6}},<ref name="MPEC-2000-L09"/><ref name="MPC-object"/> which is close to the Virgo constellation's coordinates around {{RA|13}} and {{Dec|0}}.<ref name="Virgo-coords"/>}} The subtle movement of Huya was detected by the QUEST's computer program, which was designed to identify moving objects by [[Earth:Superimposition|superimposing]] multiple images.<ref name="Ferrin2001"/><ref name="YaleNews"/> 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.<ref name="Ferrin2001"/>

The discovery of Huya was formally announced by the [[Organization:Minor Planet Center|Minor Planet Center]] in a [[Organization:Minor Planet Center#Publications|Minor Planet Electronic Circular]] on 3 June 2000.<ref name="MPEC-2000-L09"/> It was given the [[Astronomy:Provisional designation|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.<ref name="designation"/> The last letter and numbers of its designation indicate that Huya is the 4327th object discovered in the first half of March.<ref name="designation"/> At that time, Huya was thought to be one of the largest [[Astronomy:Minor planet|minor planet]]s in the [[Astronomy:Solar System|Solar System]] due to its [[Astronomy:Apparent magnitude|apparent magnitude]] of 20, which is relatively bright for a distant object.<ref name="Ferrin2001"/> This implied that it might be around one-fourth the size of [[Astronomy:Pluto|Pluto]] and comparable in size to the [[Astronomy:Dwarf planet|dwarf planet]] {{dp|Ceres}}.<ref name="YaleNews"/><ref name="NYT-20001026"/><ref name="NYT-20001107"/> Baltay, leader of the discovery team and chairman of [[Organization:Yale University|Yale University]]'s Department of Physics, proclaimed that the discovery was significant because it was the largest object discovered in the [[Astronomy:Kuiper belt|Kuiper belt]] since Pluto in 1930.<ref name="YaleNews"/> 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.<ref name="NYT-20001026"/><ref name="YaleNews"/>}}

After the announcement of Huya's discovery, the discovery team found [[Astronomy:Precovery|precovery image]]s of Huya taken with the [[Organization:Palomar Observatory|Palomar Observatory]]'s [[Astronomy:Samuel Oschin telescope|Samuel Oschin telescope]] on 9 April 1996.<ref name="Ferrin2001"/><ref name="MPC-object"/> These precovery images of Huya from Palomar are the earliest known observations of Huya.<ref name="MPC-object"/><ref name="jpldata"/> The precovery images along with subsequent follow-up observations in 2000 extended Huya's [[Astronomy:Observation arc|observation arc]] up to four years, which helped refine Huya's orbit.<ref name="Ferrin2001"/> By 2002, Huya was observed 303 times.<ref name="MPC45213"/> This was sufficient to accurately determine its orbit, so was assigned the [[Astronomy:Minor planet number|minor planet number]] 38628 to Huya on 28 March 2002.<ref name="MPC45213"/><ref name="Nomenclature"/>

=== 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.<ref name="MPC48397"/><ref name="IPS-News"/> 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.<ref name="GuajiroLiterature"/> Juyá is also associated with the winter and lives in the celestial altitudes beyond the sun.<ref name="Schmadel2006"/> 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.<ref name="IPS-News"/> Ferrín presumed that Huya had experienced multiple [[Astronomy:Impact event|impact event]]s during its formation, which he considered analogous to rain, a trait associated with Juyá.<ref name="IPS-News"/>

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.<ref name="IPS-News"/> Among 20 potential names considered by Ferrín's team, they chose the name ''Juyá'', altered to its equivalent phonetic English spelling ''Huya''.<ref name="IPS-News"/> The name was later submitted and proposed to the [[Organization:International Astronomical Union|International Astronomical Union]] (IAU), which then approved the name in 2003.<ref name="MPC48397"/> The Minor Planet Center published the naming citation on 1 May 2003.<ref name="MPC48397"/> Although the IAU's present [[Astronomy:Astronomical naming conventions#Minor planets|naming convention for minor planets]] requires objects in the orbital class of [[Astronomy:Plutino|plutino]]s (objects in 3:2 orbital resonance with [[Astronomy:Neptune|Neptune]]) to be named after underworld deities,<ref name="Nomenclature"/> these guidelines had not yet been established when Huya was named.<ref name="Nomenclature-archive"/>

== Orbit ==
[[File:AnimatedOrbitOf38628Huya.gif|thumb|upright|Polar view of Huya's orbit around the Sun, with the outer planets' orbits shown for comparison.]]
Huya is in a 2:3 [[Astronomy:Mean motion|mean-motion]] orbital resonance with Neptune, meaning that Huya completes two orbits around the Sun for every three orbits completed by Neptune.<ref name="MPEC-2006-D28"/> Due to its 2:3 orbital resonance with Neptune, Huya is classified as a [[Astronomy:Plutino|plutino]], a dynamical class of objects with orbits similar to that of Pluto.<ref name="Ferrin2001"/> Huya orbits the [[Astronomy:Sun|Sun]] at an average distance of {{convert|39.8|AU|km|lk=in|abbr=on}}, taking 250 years to complete a full orbit.<ref name="jpldata"/> Huya's orbit is [[Astronomy:Orbital inclination|inclined]] to the [[Astronomy:Ecliptic|ecliptic]] by 15.5&nbsp;[[Degree (angle)|degrees]], slightly less than Pluto's orbital inclination of 17&nbsp;degrees.<ref name="jpldata"/><ref name="johnston-list"/> It has an elongated orbit with an [[Astronomy:Orbital eccentricity|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&nbsp;AU at perihelion (closest distance) to 51.1&nbsp;AU at aphelion (farthest distance).<ref name="jpldata"/> Like Pluto, its resonance with Neptune prevents close approaches between Huya and the giant planets.<ref name="Pluto-orbit"/> The [[Astronomy:Minimum orbit intersection distance|minimum orbit intersection distance]] (MOID) between Huya and Neptune is 1.45 AU,<ref name="MPC-object"/> but due to the resonance, the two never come closer than 21 AU of each other.

Huya passed perihelion in December 2014,<ref name="Horizons2014"/> 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.<ref name="AstDyS_now"/><ref name="SkyMap"/> Simulations by the [[Astronomy:Deep Ecliptic Survey|Deep Ecliptic Survey]] (DES) show that Huya can acquire a perihelion distance (''q<sub>min</sub>'') as small as 27.27&nbsp;AU over the next 10 million years.<ref name="Buie"/>
{{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 [[Astronomy:Neptune|Neptune]], [[Astronomy:Pluto|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}}

== Physical characteristics ==
=== Size ===
{| class="wikitable floatleft" style="text-align: center; font-size: 0.9em; margin-right: 12px;"
|+ Size estimates for Huya
!Year!!Diameter (km)!!Method!!Refs
|-
|2001
|{{val|600|p=~}}
|assumed albedo
|<ref name="Ferrin2001"/>
|-
|2003
|{{val|540|p=<}}
|photometry
|<ref name="Altenhoff2004"/>
|-
|2005
|{{val|548|p=<}}
|thermal
|<ref name="Grundy2005"/>
|-
|2005
|{{val|480|50}}
|thermal
|<ref name="Stansberry2005"/>
|-
|2007
|{{val|546.5|47.8|47.1}}<br/>''or'' {{val|523.1|22.7|21.9}}
|thermal<br/>{{small|(Spitzer 2-Band)}}
|<ref name="Stansberry2008"/>
|-
|2007
|{{val|532.6|24.4|25.1}}
|thermal<br/>{{small|(adopted)}}
|<ref name="Stansberry2008"/>
|-
|2012
|{{val|438.7|26.5|25.2}}
|thermal
|<ref name="TNOsCool5"/>
|-
|2012
|{{val|384|98|134}}
|photometry
|<ref name="Sekiguchi2012"/>
|-
|2013
|{{val|438.5|0.5}}
|best-fit albedo
|<ref name="Mommert2013"/>
|-
|2013
|{{val|458|9.2}}<br/>''or'' {{val|406|16}} {{small|(primary only)}}
|thermal
|<ref name="TNOsCool8"/>
|-
|2019
|{{val|458|22|21}}
|thermal
|<ref name="Lellouch2019"/>
|-
|2019
|{{val|411.0|7.3}}
|stellar occultation
|<ref name="Santos-Sanz-2022"/>
|}
[[File:38628 Huya render.png|thumb|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.<ref name="Grundy2019"/>]]
At the time of discovery, Huya was thought to be about one-fourth the size of Pluto, or {{convert|600|km|mi|abbr=on}} in size, based on an initially measured bright [[Astronomy:Absolute magnitude|absolute magnitude]] of 4.7 and an assumed dark [[Earth:Albedo|albedo]] (reflectivity) of 0.04.<ref name="Ferrin2001"/> 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.{{efn|Pluto was still considered a planet at the time.}}<ref name="Ferrin2001"/><ref name="YaleNews"/><ref name="NYT-20001107"/> Subsequent measurements of Huya's thermal emission yielded higher albedo estimates for Huya, consequently corresponding to smaller diameter estimates.<ref name="johnston-tnos"/> [[Astronomy:Photometry|Photometric]] and thermal observations of Huya in 2003 and 2005 placed an upper limit to Huya's diameter at {{convert|540|-|548|km|mi|abbr=on}}, based on a minimum albedo around 0.08.<ref name="Altenhoff2004"/><ref name="Grundy2005"/>

Early estimates for Huya's diameter were calculated from its apparently high [[Astronomy:Absolute magnitude|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.<ref name="johnston-tnos"/><ref name="TNOsCool8"/><ref name="IAUC9253"/> By subtracting the satellite's effects from Huya's brightness, astronomers were able to approximate Huya's true diameter.<ref name="TNOsCool8"/> Huya's mean diameter is estimated at {{convert|406|km|mi|abbr=on}}, based on measurements of Huya's thermal emission by the [[Astronomy:Herschel Space Observatory|Herschel Space Observatory]] in 2013.<ref name="TNOsCool8"/> Compared to Pluto and its moon [[Astronomy:Charon (moon)|Charon]], Huya is approximately one-sixth the diameter of Pluto and one-third the diameter of Charon.{{efn|The current estimates of Pluto and Charon's diameters are {{val|2376|u=km}} and {{val|1212|u=km}}, respectively.<ref name="Stern2018"/> One-sixth of Pluto's diameter is {{val|396|u=km}} and one-third of Charon's diameter is {{val|404|u=km}}, close to the 2013 Herschel estimate of {{val|406|16|u=km}} for Huya's diameter.}}

On 18 March 2019, Huya [[Astronomy:Occultation|occulted]] a bright 10.6-[[Astronomy:Magnitude|magnitude]] star, briefly dimming the star as Huya passed in front of it.<ref name="Santos-Sanz-2019"/><ref name="Santos-Sanz-2022"/><ref name="occultation-prediction"/> The stellar occultation was observed by astronomers across [[Place:Central Europe|central Europe]] and [[Earth:Asia|Asia]] and was detected by 21 telescopes at 18 observation sites in the region.<ref name="Santos-Sanz-2022"/> Successful detections of the occultation yielded 14 [[Astronomy:Chord|chord]]s from Romania, three chords from [[Place:Turkey|Turkey]], and three chords from [[Place:Israel|Israel]].<ref name="Santos-Sanz-2022"/> 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 {{val|435.2|7.0}} by {{val|388.2|12.2|u=km}} at the time of the occultation.<ref name="Santos-Sanz-2019"/><ref name="Santos-Sanz-2022"/> Assuming that Huya is a [[Astronomy:Maclaurin spheroid|Maclaurin spheroid]], it would be approximately 435 by 435 by 233&nbsp;km in size, with a density of about {{val|800|u=g/cm3}}.<ref name="Santos-Sanz-2022"/> 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.<ref name="Santos-Sanz-2019"/><ref name="Santos-Sanz-2022"/> Rings with a width smaller than 0.1&nbsp;km, or an opacity of less than 50 percent, remain possible.<ref name="Santos-Sanz-2022"/>

==== 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.<ref name="johnston-tnos"/><ref name="Tancredi2008"/> Astronomer Gonzalo Tancredi considered Huya as a [[Astronomy:List of possible dwarf planets#Tancredi's assessment|possible dwarf planet]] with an estimated diameter larger than {{convert|450|km|mi|abbr=on}}, the suggested minimum size for icy objects to maintain a [[Spheroid|spheroid]]al shape.<ref name="Tancredi2008"/><ref name="Tancredi2010"/> However, later measurements of Huya's diameter yielded smaller size estimates, casting doubt on this possibility.<ref name="johnston-tnos"/> Adopting Herschel's mean diameter estimate of {{convert|406|km|mi|abbr=on}},<ref name="TNOsCool8"/> Huya is slightly larger than [[Astronomy:Saturn|Saturn]]'s moon Mimas, which is ellipsoidal in shape, and slightly smaller than Neptune's moon [[Astronomy:Proteus (moon)|Proteus]], which is irregular in shape.{{efn|Mimas has a mean diameter of {{convert|396|km|mi|abbr=on}} and Proteus has a mean diameter of {{convert|420|km|mi|abbr=on}}.<ref name="jplssd"/> Adopting Herschel's mean diameter estimate of {{convert|406|km|mi|abbr=on}} for Huya, it is larger than Mimas and smaller than Proteus.}} In 2019, William Grundy and colleagues proposed that trans-Neptunian objects in the size range of approximately {{convert|400|-|1000|km|mi|abbr=on}} are transitional between smaller, porous (and thus low-density) bodies and larger, denser, brighter and geologically differentiated planetary bodies such as dwarf planets.<ref name="Grundy2019"/> Huya is situated at the lower end of the size range, implying that Huya's interior structure is likely highly [[Earth:Porosity|porous]] and [[Astronomy:Planetary differentiation|undifferentiated]] since its formation and thus is unlikely to be in [[Astronomy:Hydrostatic equilibrium|hydrostatic equilibrium]].<ref name="Grundy2019"/> In a 2014 study, Audrey Thirouin and colleagues had suggested that the minimum density of Huya was {{val|1.43|u=g/cm3}}, but this was a rough estimate derived indirectly from variations in brightness.<ref name="Thirouin2014"/> Based on a 2019 stellar occultation, Santos-Sanz et al. found a density of about {{val|0.8|u=g/cm3}} if Huya is a [[Astronomy:Maclaurin spheroid|Maclaurin spheroid]], and {{val|0.859|u=g/cm3|p=>}} if it is a [[Astronomy:Jacobi ellipsoid|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".<ref name="Santos-Sanz-2022"/>

=== Spectra and surface ===
The [[Physics:Reflectance|reflectance]] [[Spectrum|spectrum]] of Huya appears moderately red and featureless in the infrared spectrum, lacking apparent [[Physics:Spectral line|absorption signature]]s of [[Earth:Ice|water ice]] and other [[Earth:Volatile (astrogeology)|volatile material]]s.<ref name="Jewitt2001"/><ref name="deBergh2004"/><ref name="TNOsCool8"/> The [[Astronomy:Scattered disc|scattered disc]] object {{mpl|1996 TL|66}} shares a similarly featureless spectrum with Huya, though their visible colors differ.<ref name="Brown2000"/> Huya's featureless spectrum indicates that its surface is covered with a thick layer of dark [[Chemistry:Organic compound|organic compound]]s irradiated by solar radiation and [[Astronomy:Cosmic ray|cosmic ray]]s.<ref name="Brown2000"/><ref name="Licandro2001"/> Although water ice appears to be absent in Huya's infrared spectrum, some astronomers have detected subtle signs of water ice in its [[Physics:Visible spectrum|visible spectrum]] in 2011 and 2017.<ref name="Barucci2011"/><ref name="Merlin2017"/> The discrepancy of the presence of water ice between the visible and infrared spectra of Huya was interpreted as an indication of [[Chemistry:Homogeneity and heterogeneity|heterogeneity]] in Huya's surface composition.<ref name="TNOsCool8"/> 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.<ref name="Merlin2017"/> Early observations of Huya's spectrum in 2000 have identified a red [[Spectral slope|spectral slope]] at [[Wavelength|wavelength]]s around 0.7&nbsp;μm, typical of dark trans-Neptunian objects.<ref name="Ferrin2001"/> Additional near-infrared absorption features were also identified, and were attributed to the presence of [[Chemistry:Aqueous solution|aqueously]] altered [[Chemistry:Silicate|silicate]] minerals on Huya's surface.<ref name="Licandro2001"/><ref name="deBergh2004"/>

The red color of Huya's surface results from the irradiation of organic compounds by solar radiation and cosmic rays, which produces dark, reddish [[Astronomy:Tholin|tholin]]s that cover its surface.<ref name="Licandro2001"/> 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.<ref name="Licandro2001"/> Compared to the large Kuiper belt object {{dp|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.<ref name="Licandro2001"/> 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.<ref name="Licandro2001"/> Best-fit models for these absorption features suggest that Huya's surface consists of a mixture of [[Astronomy:Comet|comet]]ary ice tholins (ice tholin II),<ref name="McDonald1996"/> [[Chemistry:Nitrogen|nitrogen]]-rich [[Astronomy:Tholin#Titan|Titan tholin]]s,<ref name="McDonald1994"/> as well as water ice.<ref name="deBergh2004"/>

[[Astronomy:Spectrograph|Spectrograph]]ic observations of Huya's spectrum with the [[Astronomy:Very Large Telescope|Very Large Telescope]] in 2001 and 2002 have tentatively identified weak absorption features at near-infrared wavelengths around 0.6–0.82&nbsp;μm, possibly indicating the presence of phyllosilicate materials on its surface.<ref name="deBergh2004"/> The 0.6&nbsp;μm absorption feature in Huya's spectrum resembles those in the spectra of stony [[Astronomy:S-type asteroid|S-type asteroid]]s, which may suggest the presence of [[Chemistry:Spinel group|spinel group]] minerals, albeit in trace amounts as such minerals are unlikely to be abundant in trans-Neptunian objects.<ref name="deBergh2004"/> Other absorption features near 0.7&nbsp;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 [[Physics:Radioactive decay|radioactive decay]] of [[Physics:Radionuclide|radionuclide]]s in Huya's interior.<ref name="deBergh2004"/> 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.<ref name="Merlin2017"/>

==== Brightness ====
Huya has a visual [[Astronomy:Absolute magnitude#Solar System bodies (H)|absolute magnitude]] (H) of 5.04 and a low [[Physics:Geometric albedo|geometric albedo]] of 0.083.<ref name="TNOsCool8"/> Its [[Astronomy:Apparent magnitude|apparent magnitude]], the brightness as seen from Earth, varies from 19.8 to 21.6 magnitudes.<ref name="Grundy-orbits"/> Huya comes to [[Astronomy:Opposition (planets)|opposition]] in June of each year at a visual [[Astronomy:Apparent magnitude|apparent magnitude]] of 19.8.<ref name="Grundy-orbits"/><ref name="AstDys"/> At wavelengths of the [[Astronomy:Photometric system|R-band]] range, Huya appears brighter in red light,<ref name="Ferrin2001"/> with its R-band apparent magnitude reaching 19.11 magnitudes at opposition.<ref name="Schaefer2002"/> 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.<ref name="Ferrin2001"/> As Huya comes to opposition, its brightness increases as a result of an [[Physics:Opposition surge|opposition surge]], in which its [[Physics:Phase angle|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.<ref name="Schaefer2002"/> Huya appeared to display very little variability in brightness, with an estimated [[Astronomy:Light curve|light curve]] [[Physics:Amplitude|amplitude]] of less than 0.097 magnitudes.<ref name="Schaefer2002"/>

== Rotation ==
The [[Rotation period|rotation period]] of Huya is unknown due to the flat appearance of its light curve, displaying very little variability in brightness.<ref name="IAUC7459"/><ref name="Sheppard2002"/><ref name="Sheppard2008"/> 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.<ref name="IAUC7459"/><ref name="Ferrin2001"/> 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.<ref name="Schaefer2002"/> 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.<ref name="Ortiz2003"/> 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.<ref name="Thirouin2014"/> 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 [[Physics:Tidal force|tidal force]]s 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.<ref name="Ortiz2003"/><ref name="Thirouin2014"/><ref name="Galiazzo2016"/>

In 2002, [[Biography:José Luis Ortiz Moreno|Ortiz]] and colleagues obtained a fragmentary rotation period of {{val|6.75|0.01}} hours for Huya, along with other alternative periods of {{val|6.68|0.01}} and {{val|6.82|0.01}} hours.<ref name="Ortiz2003"/> Their inferred rotation period was derived from [[Data set|data set]]s of short-term photometry taken separately in February and March 2002.<ref name="Ortiz2003"/> Their mean solution of {{val|6.75|0.01}} for Huya's rotation period appeared consistent with previous photometric observations, with an amplitude less than 0.1 magnitudes.<ref name="Ortiz2003"/> However, the rotation period determined by Ortiz was later determined to be an [[Aliasing|alias]] of Huya's brightness variability.<ref name="Thirouin2014"/> 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.<ref name="Thirouin2014"/> 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.<ref name="jpldata"/>

== Exploration ==
In a study published by Ashley Gleaves and colleagues in 2012, Huya was considered as a potential target for an [[Engineering:Orbiter|orbiter]] mission that would be launched on an [[Engineering:Atlas V|Atlas V 551]] or [[Engineering:Delta IV|Delta IV HLV]] rocket. For an orbiter mission to Huya, the spacecraft would have a launch date in November 2027 and use a [[Astronomy:Gravity assist|gravity assist]] from Jupiter, taking 20 to 25 years to arrive.<ref name="Gleaves2012"/> 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.<ref name="Gleaves2012"/> For a [[Engineering:Flyby (spaceflight)|flyby]] mission to Huya, [[Astronomy:Planetary science|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.<ref name="Zangari2018"/> 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.<ref name="Zangari2018"/>

== Satellite ==
{{Infobox planet
 | name            = S/2012 (38628) 1
 | image           = File:38628-huya.gif
 | image_scale      =
 | caption         = Hubble images of Huya and its satellite, taken one day apart between June and July 2002
 | discovery_ref   = <ref name="IAUC9253"/>
 | discoverer      = Keith S. Noll<br/>William M. Grundy<br/>Hilke Schlichting<br/>Ruth Murray-Clay<br/>Susan D. Benecchi
 | discovered      = 6 May 2012<br/>(announced on 12 July 2012)
 | satellite_of    = Huya
 | orbit_ref       = <ref name="johnston"/>
 | epoch           = 
 | semimajor       = {{val|1740|80|u=km|p=~}} {{small|(projected distance)}}
 | period          = {{val|3.2|u=d|p=~}} {{small|(assumed)}}
 | eccentricity    = 
 | inclination     = 
 | asc_node        = 
 | arg_peri        = 
 | physical_ref    = <ref name="TNOsCool8"/>
 | mean_diameter   = {{val|213|30|u=km}} {{small|(assuming the same albedo as the primary)}}
 | density         = 
 | albedo          = 0.083 (assumed)
 | abs_magnitude   = 6.44
}}

'''S/2012 (38628) 1''' is the [[Astronomy:Provisional designation#Moons of minor planets|provisional designation]] for the only known satellite of Huya.<ref name="IAUC9253"/><ref name="johnston"/> It was discovered by a team led by Keith Noll in [[Astronomy:Hubble Space Telescope|Hubble Space Telescope]] observations obtained on 6 May 2012, and confirmed in reexamination of [[Astronomy:Precovery|archival]] Hubble Space Telescope imagery from 30 June and 1 July 2002.<ref name="IAUC9253"/> The discovery was reported to the International Astronomical Union and was announced on 12 July 2012.<ref name="IAUC9253"/> Assuming the same albedo as Huya, the satellite is estimated to be about {{convert|213|km|mi|abbr=on}} in diameter.<ref name="TNOsCool8"/> From Hubble images of Huya, the satellite's separation distance from the primary is estimated to be at least {{convert|1740|km|mi|abbr=on}}.<ref name="johnston"/>

=== Characteristics ===
The satellite is 1.4 magnitudes dimmer than Huya (H<sub>V</sub>=5.04),<ref name="IAUC9253"/> giving a visual absolute magnitude of 6.44 for the satellite.<ref name="TNOsCool8"/>{{efn|A larger magnitude value corresponds to a dimmer brightness.}} The satellite is relatively large compared to Huya, being slightly larger than half the primary's diameter of {{convert|406|km|mi|abbr=on}}.<ref name="johnston"/><ref name="TNOsCool8"/> The size ratio of the satellite to the primary is 0.525.<ref name="johnston"/> The large size ratio is analogous to the Pluto–Charon [[Astronomy:Binary system|binary system]], in which Pluto's large moon [[Astronomy:Charon (moon)|Charon]] is large and massive enough such that the [[Barycenter|center of mass]] (barycenter) is located in the space between Charon and Pluto.<ref name="Stern2018"/><ref name="Thirouin2014"/> The Huya system may be in a similar case, although no information about its barycenter is known.<ref name="Thirouin2014"/> 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,<ref name="Thirouin2014"/> although several photometric observations of Huya indicate a rotation period of several hours, suggesting that Huya may not be tidally locked to its satellite.<ref name="Ortiz2003"/><ref name="Galiazzo2016"/> If Huya is not tidally locked to its satellite, this implies that the satellite could have a very low density of around {{val|0.5|u=g/cm3}}, which would result in a longer time for both components to become mutually tidally locked.<ref name="Thirouin2014"/>

The orbit of the satellite is poorly known due to the small number of resolved observations of Huya's satellite.<ref name="Grundy-orbits"/> Consequently, a definitive mass and density estimate for Huya cannot be derived from the satellite's orbit.<ref name="TNOsCool8"/> Based on archival Hubble images of Huya taken in 2002, the satellite's [[Astronomy:Angular distance|angular separation]] distance from Huya is approximately 60 to 80 milliarcseconds,<ref name="IAUC9253"/><ref name="Grundy-orbits"/> corresponding to an approximate distance of {{val|1740|80|u=km}}.<ref name="johnston"/> The orbital period of the satellite is estimated at about 3.2 days.<ref name="johnston"/>

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

== References ==
{{Reflist|30em|refs=

<ref name="jpldata">{{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  = [[Organization:Jet Propulsion Laboratory|Jet Propulsion Laboratory]]
 |date       = 13 July 2019
 |access-date = 20 February 2020}}</ref>

<ref name="Schmadel2006">{{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 }}</ref>

<ref name="MPC-object">{{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}}</ref>

<ref name="MPEC-2000-L09">{{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}}</ref>

<ref name="MPEC-2006-D28">{{cite web
 |title      = MPEC 2006-D28 : DISTANT MINOR PLANETS (2006 MAR. 26.0 TT)
 |publisher  = International Astronomical Union
 |work       = Minor Planet Center
 |url        = https://minorplanetcenter.net//mpec/K06/K06D28.html
 |date       = 23 February 2006
 |access-date = 22 October 2019}}</ref>

<ref name="MPC45213">{{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}}</ref>

<ref name="MPC48397">{{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}}</ref>

<ref name="lcdb">{{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}}</ref>

<ref name="AstDys">{{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}}</ref>

<ref name="Horizons2014">{{cite web
  |title=Horizons Batch for 38628 Huya on 2014-Dec-14
  |publisher=[[Astronomy:JPL Horizons On-Line Ephemeris System|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
  |accessdate=2023-08-27}} (JPL#42/Soln.date: 2023-Jul-28)</ref>

<ref name="Brown2000">{{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
 }}</ref>

<ref name="Licandro2001">{{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 }}</ref>

<ref name="Jewitt2001">{{cite journal
 |title=Colors and Spectra of Kuiper Belt Objects
 |first1=David C. |last1=Jewitt
 |first2=Jane X. |last2=Luu
 |date=2001
 |journal=The Astronomical Journal
 |volume=122
 |number=4
 |pages=2099–2114
 |doi=10.1086/323304
 |arxiv=astro-ph/0107277 |bibcode=2001AJ....122.2099J|s2cid=35561353 |url=https://cds.cern.ch/record/509438
 }}</ref>

<ref name="Sheppard2002">{{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
 }}</ref>

<ref name="Schaefer2002">{{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 }}</ref>

<ref name="Ortiz2003">{{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
 }}</ref>

<ref name="Altenhoff2004">{{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}}</ref>

<ref name="Grundy2005">{{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 }}</ref>

<ref name="Stansberry2005">{{cite conference
 |title=Albedos, Diameters (and a Density) of Kuiper Belt and Centaur Objects
 |first1=J. A. |last1=Stansberry
 |first2=D. P. |last2=Cruikshank
 |first3=W. G. |last3=Grundy
 |first4=J. L. |last4=Margot
 |first5=J. P. |last5=Emery
 |first6=Y. R. |last6=Fernández
 |first7=G. H. |last7=Reike
 |date=August 2005
 |conference=37th DPS Meeting
 |publisher=American Astronomical Society
 |volume=37
 |page=737
 |id=52.05
 |bibcode=2005DPS....37.5205S}}</ref>

<ref name="Rabinowitz2006">{{cite journal
 |title=The Diverse Solar Phase Curves of Distant Icy Bodies. I. Photometric Observations of 18 Trans-Neptunian Objects, 7 Centaurs, and Nereid
 |first1=David L. |last1=Rabinowitz
 |first2=Bradley E. |last2=Schaefer
 |first3=Suzanne W. |last3=Tourtellote
 |journal=The Astronomical Journal
 |volume=133
 |pages=26–43
 |number=1
 |date=2007
 |doi=10.1086/508931
 |arxiv=astro-ph/0605745
 |bibcode=2007AJ....133...26R|s2cid=119406900 }}</ref>

<ref name="Buie">{{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=[[Organization:Southwest Research Institute|Southwest Research Institute]]
 |access-date=17 July 2008}}</ref>

<ref name="deBergh2004">{{cite journal
 |title=Aqueous altered silicates at the surface of two Plutinos?
 |url=https://www.aanda.org/articles/aa/pdf/2004/11/aa3543.pdf
 |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=10.1051/0004-6361:20031727
 |bibcode=2004A&A...416..791D}}</ref>

<ref name="Barucci2011">{{cite journal
 |title=New insights on ices in Centaur and Transneptunian populations
 |url=https://pdfslide.net/documents/new-insights-on-ices-in-centaur-and-transneptunian-populations.html
 |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
 |first7=F. |last7=DeMeo
 |first8=S. |last8=Fornasier
 |journal=Icarus
 |volume=214
 |issue=1
 |pages=297–307
 |date=July 2011
 |doi=10.1016/j.icarus.2011.04.019
 |bibcode=2011Icar..214..297B|s2cid=120331897
 }}</ref>

<ref name="TNOsCool8">{{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=0
 |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
 }}</ref>

<ref name="Cruikshank2007">{{cite book
 |first1=D. P. |last1=Cruikshank
 |first2=M. A. |last2=Barucci
 |first3=J. P. |last3=Emery
 |first4=Y. R. |last4=Fernández
 |first5=W. M. |last5=Grundy
 |first6=K. S. |last6=Noll
 |first7=J. A. |last7=Stansberry
 |date=2007
 |chapter-url=https://www.lpi.usra.edu/books/PPV/8050.pdf
 |chapter=Physical Properties of Transneptunian Objects
 |title=Protostars and Planets V
 |publisher=University of Arizona Press
 |pages=879–893
 |isbn=978-0-8165-2755-7
 |bibcode=2007prpl.conf..879C}}</ref>
<!-- https://www.lpi.usra.edu/books/PPV/download.html -->

<ref name="Sheppard2008">{{cite book
 |title=The Solar System Beyond Neptune
 |chapter-url=http://web.gps.caltech.edu/~mbrown/out/kbbook/Chapters/Sheppard_Lightcurves.pdf
 |first1=S. S. |last1=Sheppard
 |first2=P. |last2=Lacerda
 |first3=J. L. |last3=Ortiz
 |date=2008
 |editor-first=A. M. |editor-last=Barucci
 |chapter=Photometric Lightcurves of Transneptunian Objects and Centaurs: Rotations, Shapes, and Densities
 |publisher=University of Arizona Press
 |pages=129–142
 |bibcode=2008ssbn.book..129S
 |isbn=978-0-8165-2755-7}}</ref>

<ref name="Stansberry2008">{{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}}</ref>
<!-- https://www.lpi.usra.edu/books/ssbn2008/download.html -->

<ref name="Tancredi2008">{{cite web
 |last1=Tancredi |first1=G.
 |last2=Favre |first2=S.
 |date=2008
 |title=Which are the dwarfs in the solar system?
 |publisher=Asteroids, Comets, Meteors
 |url=http://www.lpi.usra.edu/meetings/acm2008/pdf/8261.pdf
 |access-date=16 October 2019}}</ref>

<ref name="Tancredi2010">{{cite journal
 |first=Gonzalo |last=Tancredi
 |title=Physical and dynamical characteristics of icy "dwarf planets" (plutoids)
 |journal=Proceedings of the International Astronomical Union
 |date=6 April 2010
 |volume=5
 |issue=S263
 |pages=173–185
 |bibcode=2010IAUS..263..173T
 |doi=10.1017/S1743921310001717|doi-access=free
 }}</ref>

<ref name="Sekiguchi2012">{{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
 |first7=T. G. |last7=Müller
 |date=May 2012
 |conference=Asteroids, Comets, Meteors
 |publisher=Lunar and Planetary Institute
 |issue=1667
 |id=6477
 |bibcode=2012LPICo1667.6477S}}</ref>

<ref name="Ferrin2001">{{cite journal
 |title=Discovery of the Bright Trans-Neptunian Object {{mp|2000 EB|173}}
 |display-authors=0
 |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=10.1086/319109
 |arxiv=astro-ph/0011527|s2cid=16937417
 }}</ref>
<!-- archived paper published by Yale University in https://archive.today/20001204154300/http://hepwww.physics.yale.edu/www_info/astro/papers/eb173_paper_rev2.html -->

<ref name="Gleaves2012">{{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
 |journal=AIAA/AAS Astrodynamics Specialist Conference
 |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}}</ref>

<ref name="TNOsCool5">{{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=0
 |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
 }}</ref>

<ref name="Thirouin2014">{{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
 }}</ref>

<ref name="Belskaya2015">{{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}}</ref>

<ref name="Galiazzo2016">{{cite journal
 |title=Photometry of Centaurs and trans-Neptunian objects: 2060 Chiron (1977 UB), 10199 Chariklo ({{mp|1997 CU|26}}), 38628 Huya ({{mp|2000 EB|173}}), 28978 Ixion ({{mp|2001 KX|76}}), and 90482 Orcus (2004 DW)
 |first1=M. |last1=Galiazzo
 |first2=C. |last2=de la Fuente Marcos
 |first3=R. |last3=de la Fuente Marcos
 |first4=G. |last4=Cararro
 |first5=M. |last5=Maris
 |first6=M. |last6=Montalto
 |date=July 2016
 |journal=Astrophysics and Space Science
 |volume=361
 |issue=212
 |doi=10.1007/s10509-016-2801-5
 |arxiv=1605.08251
 |s2cid=119204060 |issn=1572-946X}}</ref>

<ref name="Merlin2017">{{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
 }}</ref>

<ref name="Zangari2018">{{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 }}</ref>

<ref name="Lellouch2019">{{cite journal
 |title=The thermal emission of Centaurs and Trans-Neptunian objects at millimeter wavelengths from ALMA observations
 |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
 |first7=M. |last7=Gurwell
 |first8=J. |last8=Stansberry
 |first9=R. |last9=Leiva
 |first10=B. |last10=Sicardy
 |first11=B. |last11=Butler
 |first12=J. |last12=Boissier
 |date=September 2019
 |journal=Monthly Notices of the Royal Astronomical Society
 |volume=488
 |issue=3
 |pages=3035–3044
 |doi=10.1093/mnras/stz1880
 |arxiv=1709.06747}}</ref>

<ref name="Grundy2019">{{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
 |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}}</ref>

<ref name="Santos-Sanz-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=0
 |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}}</ref>
 
<ref name="Santos-Sanz-2022">{{cite journal
 |title=Physical properties of the trans-Neptunian object (38628) Huya from a multi-chord stellar occultation
 |url=https://www.aanda.org/articles/aa/pdf/forth/aa41546-21.pdf
 |display-authors=0
 |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=10.1051/0004-6361/202141546|bibcode=2022A&A...664A.130S
 |s2cid=249063125
 }}</ref>

<ref name="IAUC7459">{{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}}</ref>

<ref name="IAUC9253">{{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}}</ref>

<ref name="occultation-prediction">{{cite web
 |title=Occultation by Huya (2019-03-18)
 |url=http://lesia.obspm.fr/lucky-star/occ.php?p=15369
 |work=ERC Lucky Star project
 |date=13 March 2019
 |access-date=25 October 2019}}</ref>

<ref name="YaleNews">{{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=[[Organization:Yale University|Yale University]]
 |work=YaleNews
 |date=25 October 2000
 |access-date=16 October 2019}}</ref>

<ref name="NYT-20001026">{{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}}</ref>

<ref name="NYT-20001107">{{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}}</ref>

<ref name="designation">{{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}}</ref>

<ref name="Virgo-coords">{{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}}</ref>

<ref name="GuajiroLiterature">{{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=[[Organization:University of California, Los Angeles|University of California, Los Angeles]]
 |volume=2
 |isbn=9780879030636
 |year=1986
 |access-date=18 October 2019}}</ref>

<ref name="IPS-News">{{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}}</ref>

<ref name="Nomenclature">{{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}}</ref>

<ref name="Nomenclature-archive">{{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=bot: unknown }}</ref>

<ref name="Grundy-orbits">{{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}}</ref>

<ref name="Mommert2013">{{cite thesis
 |title=Remnant Planetesimals and their Collisional Fragments
 |url=https://refubium.fu-berlin.de/bitstream/handle/fub188/2283/PhD_mommert_fuonline.pdf?sequence=1&isAllowed=y
 |first=Michael |last=Mommert
 |journal=Refubium
 |publisher=Freie Universität Berlin
 |doi=10.17169/refubium-6484
 |year=2013
 |access-date=24 October 2019}}</ref>

<ref name="Stern2018">{{cite journal
 |title=The Pluto System After New Horizons
 |display-authors=0
 |first1=S. A. |last1=Stern
 |first2=W. |last2=Grundy
 |first3=W. B. |last3=McKinnon
 |first4=H. A. |last4=Weaver
 |first5=L. A. |last5=Young
 |first6=L. A. |last6=Young
 |journal=Annual Review of Astronomy and Astrophysics
 |volume=56
 |pages=357–392
 |date=September 2018
 |doi=10.1146/annurev-astro-081817-051935
 |arxiv=1712.05669
 |bibcode=2018ARA&A..56..357S|s2cid=119072504
 }}</ref>

<ref name="jplssd">{{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}}</ref>
 
<ref name="AstDyS_now">{{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}}</ref>

<ref name="johnston">{{cite web
 |first=Wm. Robert |last=Johnston
 |work=Johnston's Archive
 |date=21 September 2014
 |title=(38628) Huya
 |url=http://www.johnstonsarchive.net/astro/astmoons/am-38628.html
 |access-date=31 October 2019}}</ref>

<ref name="johnston-tnos">{{cite web
 |title=TNO/Centaur diameters, albedos, and densities
 |url=http://www.johnstonsarchive.net/astro/tnodiam.html
 |work=Johnston's Archive
 |first=W. R. |last=Johnston
 |date=23 October 2018
 |access-date=23 October 2019}}</ref>

<ref name="johnston-list">{{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}}</ref>
 
<ref name="SkyMap">{{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}}</ref>

<ref name="Pluto-orbit">{{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}}</ref>

<ref name="McDonald1994">{{cite journal
 |title=Chemical Investigation of Titan and Triton Tholins
 |first1=Gene D. |last1=McDonald
 |first2=W. Reid |last2=Thompson
 |first3=Michael |last3=Heinrich
 |first4=Bishun N. |last4=Khare
 |first5=Carl |last5=Sagan
 |journal=Icarus
 |volume=108
 |issue=1
 |pages=137–145
 |year=1994
 |doi=10.1006/icar.1994.1046
 |pmid=11539478 |bibcode=1994Icar..108..137M|doi-access=free
 }}</ref>

<ref name="McDonald1996">{{cite journal
 |first1=Gene D. |last1=McDonald
 |first2=Linda J. |last2=Whited
 |first3=Cynthia |last3=DeRuiter
 |first4=Bishun N. |last4=Khare
 |first5=Archita |last5=Patnaik
 |first6=Carl |last6=Sagan
 |s2cid=35639172
 |title=Production and Chemical Analysis of Cometary Ice Tholins
 |journal=Icarus
 |volume=122
 |issue=1
 |pages=107–117
 |year=1996
 |doi=10.1006/icar.1996.0112
 |bibcode=1996Icar..122..107M|doi-access=free
 }}</ref>

<ref name="Schwamb2010">{{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=10.1088/0004-637X/720/2/1691
 |arxiv=1007.2954
 |bibcode=2010ApJ...720.1691S|s2cid=5853566 }}</ref>

}} <!-- end of reflist -->

== External links ==
* [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}}

{{Dwarf planets}}
{{Solar System moons (compact)}}
{{Trans-Neptunian objects}}
{{Small Solar System bodies}}
{{Solar System}}

{{DEFAULTSORT:Huya}}
[[Category:Plutinos|038628]]
[[Category:Possible dwarf planets|038628]]
[[Category:Named minor planets]]

{{Sourceattribution|38628 Huya}}