|Discovered by||I. R. Ferrin|
|Discovery date||10 March 2000|
|MPC designation||(38628) Huya|
|Epoch 13 January 2016 (JD 2457400.5)|
|Uncertainty parameter 2|
|Observation arc||7010 days (19.19 yr)|
|Aphelion||50.723 AU (7.5881 Tm)|
|Perihelion||28.533 AU (4.2685 Tm)|
|39.628 AU (5.9283 Tm)|
|249.47 yr (91117.9 d)|
Average orbital speed
|0° 0m 14.223s / day|
|Earth MOID||27.5533 AU (4.12192 Tm)|
|Jupiter MOID||23.3093 AU (3.48702 Tm)|
|Jupiter Tisserand parameter||5.238|
|Dimensions||±16 km 406|
|5.28 h (0.220 d)|
Sidereal rotation period
|0.083 ± 0.004|
|B−V=0.95 ± 0.05
V−R=0.57 ± 0.09
|5.04 ± 0.03
5.37 ± 0.04
|0.020″ (max)[note 1]|
38628 Huya is a trans-Neptunian object (TNO). It is a plutino, being in a 2:3 mean-motion resonance with Neptune. It has a diameter of 458.0±9.2 km, and it is possibly a dwarf planet (icy trans-Neptunian objects with a diameter above around 400 kilometres (250 mi) are expected to be spherical), although the IAU has never classified it as such. Light-curve-amplitude analysis shows only small deviations, suggesting that Huya is likely a spheroid with small albedo spots. As of 2010, astronomer Gonzalo Tancredi thought that Huya was very probably a dwarf planet.
Huya was discovered in March 2000 by Ignacio Ferrin and announced on 24 October 2000. At the time of its discovery, Huya was the brightest (and hence estimated to be the biggest) trans-Neptunian object found since Pluto. It was found using data collected at the CIDA Observatory in Venezuela.
The Spitzer Space Telescope has estimated Huya to be about 530 kilometres (330 mi) in diameter with a low albedo of around 0.05. The later termination, based on a combination of Spitzer and Herschel measurements, yielded a smaller size of ±9.2 km. 458.7 Taking into account that Huya is a binary the diameter of the primary is estimated at ±16 km. 406
Huya has a moderately red-sloped reflectance spectrum in the visible and near-infrared, suggesting a surface rich in organic material such as tholins. There is a broad absorption feature near 2 μm possibly belonging to water ice or some water-altered material. Additional absorption features may be present near 0.6–0.8 μm, which may be caused by aqueously-altered anhydrous silicates.
Orbit and rotation
Huya is currently 28.5 AU from the Sun and it came to perihelion in December 2014. This means that it is currently inside the orbit of the planet Neptune. Like Pluto, this plutino spends part of its orbit closer to the Sun than Neptune, even though their orbits are controlled by Neptune. Huya will be closer to the Sun than Neptune until about July 2029. Simulations by the Deep Ecliptic Survey (DES) show that, over the next 10 million years, Huya can acquire a perihelion distance (qmin) as small as 27.28 AU. Plutinos (15875) 1996 TP66 and (120216) 2004 EW95 get even closer to the Sun.
Huya has been observed 131 times, with precovery images back to 1996. The rotation period of Huya is unknown: although a value of 13.50 hours has been tentatively obtained from fragmentary light curve data, it may well be completely erroneous.
A satellite, reported in IAU Circular 9253 on 12 July 2012, was discovered by Keith S. Noll, William M. Grundy, Hilke E. Schlichting, Ruth Murray-Clay and Susan D. Benecchi from Hubble Space Telescope observations obtained on 6 May 2012 and confirmed in reexamination of Hubble Space Telescope imagery from 30 June-1 July 2012. It has an estimated diameter of ±30 km 213 and a separation of 1,800 kilometres (1,100 mi) from primary. Its provisional designation is S/2012 38628 Huya 1.
- Angular size at May 2015 opposition: arctan (406 km in diameter / (27.5543 AU * 597870.7 km)) = 0.020″ 149
- Buie, M. W. (22 April 2007). "Orbit Fit and Astrometric record for 38628". SwRI (Space Science Department). Retrieved 2008-07-17.
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- Brown, M. E. (23 September 2011). "How many dwarf planets are there in the outer solar system? (updates daily)". California Institute of Technology. Archived from the original on 2011-10-18. Retrieved 2011-09-23.
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- Tancredi, G. (2009). "Physical and dynamical characteristics of icy "dwarf planets" (plutoids)". Proceedings of the International Astronomical Union. 5: 173–15. Bibcode:2010IAUS..263..173T. doi:10.1017/S1743921310001717.
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- Licandro, J.; Oliva, E.; Di Martino, M. (2001). "NICS-TNG infrared spectroscopy of trans-neptunian objects 2000 EB173 and 2000 WR106". Astronomy and Astrophysics. 373 (3): L29–L32. Bibcode:2001A&A...373L..29L. arXiv: . doi:10.1051/0004-6361:20010758.
- de Bergh, C.; et al. (2004). "Aqueous altered silicates at the surface of two Plutinos?". Astronomy and Astrophysics. 416 (2): 791–798. Bibcode:2004A&A...416..791D. doi:10.1051/0004-6361:20031727.
- "38628 Huya (2000 EB173) ephemeris". JPL Small-Body Database. Jet Propulsion Laboratory. SPK-ID: 2038628. Retrieved 2009-03-23.
- Sheppard, S. S.; Lacedra, P.; Ortiz, J. L. (2008). "Photometric Lightcurves of Transneptunian Objects and Centaurs: Rotations, Shapes, and Densities". In Barucci, A. M.; et al. The Solar System Beyond Neptune (PDF). University of Arizona Press. pp. 129–142. ISBN 978-0-8165-2755-7.
- 38628 Huya at the JPL Small-Body Database
- 37th DPS: Albedos, Diameters (and a Density) of Kuiper Belt and Centaur Objects
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- From the Rain Forest to Planet Huya