38628 Huya
Artist's impression of 38628 Huya
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Discovery and designation
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| Discovered by | Ignacio Ferrin |
| Discovery date | March 10, 2000 |
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Designations
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| MPC designation | 38628 Huya |
| Pronunciation | /huːˈjɑː/ hoo-YAH |
| Named after | Huya |
| Alternate name(s) | 2000 EB173 |
| Minor planet category |
TNO Plutino[1][2] Kozai |
| Epoch January 4, 2010 (JD 2455200.5) | |
| Aphelion | 50.363 AU (7534 Gm) |
| Perihelion | 28.520 AU (4266 Gm) |
| Semi-major axis | 39.442 AU (5900 Gm) |
| Eccentricity | 0.2768 |
| Orbital period | 247.72 yr (90477 d) |
| Average orbital speed | 4.63 km/s |
| Mean anomaly | 352.38° |
| Inclination | 15.487° |
| Longitude of ascending node | 169.40° |
| Argument of perihelion | 68.169° |
| Dimensions | 532 ± 25 km[4] |
| Mass | 6.5×1019–1.8×1020 kg[5] |
| Mean density | 2.0 g/cm3 (assumed) |
| Equatorial surface gravity | 0.12–0.15? m/s2 |
| Equatorial escape velocity | 0.23–0.28? km/s |
| Sidereal rotation period |
13.5 hr(?)[3] |
| Geometric albedo | 0.05+0.005 −0.004[4] |
| Temperature | ~44 K |
| Spectral type | (moderately red) B-V=1.00; V-R=0.65[6] |
| Apparent magnitude | 19.3 (opposition)[7] |
| Absolute magnitude (H) | 5.23[4] |
| Angular diameter | 0.024" (max)[8] |
38628 Huya is a trans-Neptunian object (TNO). It is a plutino, being in a 2:3 mean motion resonance with Neptune.[1] With a Spitzer size estimate of 532 ± 25 km,[4] it is likely a dwarf planet[9] (trans-Neptunian objects with a diameter above around 400 km are expected to be spherical) although the IAU has not officially classified it as such.[10] Light-curve-amplitude analysis, which shows only small deviations, suggests that it is likely a spheroid with small albedo spots.[11] Tancredi (2010) thinks that Huya is a very probable plutoid.[12]
It was discovered in March 2000 by Ignacio Ferrin and announced on 24 October 2000. It was assigned the name Huya, after Juyá, the Wayuu rain god, in August 2003 by the International Astronomical Union (IAU).
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[edit] Physical characteristics
At the time of its discovery, Huya was the biggest and brightest trans-Neptunian object found since Pluto. It was found using data collected by at the CIDA Observatory in Venezuela. The Spitzer Space Telescope has estimated Huya to be about 530 km in diameter with a low albedo of around 0.05.[4]
The object has a red-sloped reflectance spectrum in the visible and near-infrared, suggesting a surface rich in organic material such as tholins.[13] There is a broad absorption feature near 2 μm possible 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.[14]
[edit] Orbit and rotation
Huya is currently 28.7 AU from the Sun,[7] and will come to perihelion (q=28.52 AU) in 2015.[3] This means that this dwarf-planet candidate 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.[15] 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.[1] Plutinos (15875) 1996 TP66 and (120216) 2004 EW95 get even closer to the Sun.
Given the long orbit that TNOs have around the Sun, Huya comes to opposition in early May of each year at an apparent magnitude of 19.3.[7]
Huya has been observed 131 times with precovery images back to 1996.[3] The rotation period of Huya is unknown.[16]
[edit] References
- ^ a b c d Marc W. Buie (2007-04-22). "Orbit Fit and Astrometric record for 38628". SwRI (Space Science Department). http://www.boulder.swri.edu/~buie/kbo/astrom/38628.html. Retrieved 2008-07-17.
- ^ "MPEC 2009-C70 :Distant Minor Planets (2009 FEB. 28.0 TT)". Minor Planet Center. 2009-02-10. http://www.cfa.harvard.edu/mpec/K09/K09C70.html. Retrieved 2009-03-24.
- ^ a b c d "JPL Small-Body Database Browser: 38628 Huya (2000 EB173)". 2009-06-13 last obs. http://ssd.jpl.nasa.gov/sbdb.cgi?sstr=Huya. Retrieved 2008-07-17.
- ^ a b c d e John Stansberry, Will Grundy, Mike Brown, Dale Cruikshank, John Spencer, David Trilling, Jean-Luc Margot (2007). "Physical Properties of Kuiper Belt and Centaur Objects: Constraints from Spitzer Space Telescope". University of Arizona, Lowell Observatory, California Institute of Technology, NASA Ames Research Center, Southwest Research Institute, Cornell University. arXiv:astro-ph/0702538.
- ^ Radius of 253 km and density of 0.97 = 6.5×1019 kg mass. Radius of 279 km and density of 2.0 = 1.8×1020 kg mass
- ^ Tegler, Stephen C. (2007-02-01). "Kuiper Belt Object Magnitudes and Surface Colors". http://www.physics.nau.edu/~tegler/research/survey.htm. Retrieved 2009-12-30.
- ^ a b c "AstDys (38628) Huya Ephemerides". Department of Mathematics, University of Pisa, Italy. http://hamilton.dm.unipi.it/astdys/index.php?pc=1.1.3.0&n=Huya. Retrieved 2009-03-22.
- ^ Huya Angular Size @ May 2015 Opposition: 480km dia / (27.5543AU * 149 597 870km) * 206265 = 0.024"
- ^ Michael E. Brown (Sep 23 2011). "How many dwarf planets are there in the outer solar system? (updates daily)". California Institute of Technology. http://www.gps.caltech.edu/~mbrown/dps.html. Retrieved 2011-09-23.
- ^ Mike Brown. "The Dwarf Planets". http://web.gps.caltech.edu/~mbrown/dwarfplanets/. Retrieved 2008-01-20.
- ^ Tancredi, G., & Favre, S. (2008) Which are the dwarfs in the Solar System?. Depto. Astronomía, Fac. Ciencias, Montevideo, Uruguay; Observatorio Astronómico Los Molinos, MEC, Uruguay. Retrieved 10-08-2011
- ^ Tancredi, G. (2010). "Physical and dynamical characteristics of icy “dwarf planets” (plutoids)". Icy Bodies of the Solar System: Proceedings IAU Symposium No. 263, 2009. http://journals.cambridge.org/article_S1743921310001717.
- ^ Licandro (07/2001). NICS-TNG infrared spectroscopy of trans-neptunian objects 2000 EB173 and 2000 WR106. Astronomy and Astrophysics, v.373, p.L29-L32 (2001). Bibcode 2001astro.ph..5434L.
- ^ de Bergh, C.; Boehnhardt, H.; Barucci, M.A. 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.
- ^ "Horizon Online Ephemeris System". California Institute of Technology, Jet Propulsion Laboratory. http://ssd.jpl.nasa.gov/horizons.cgi?find_body=1&body_group=sb&sstr=Huya. Retrieved 2009-03-23.
- ^ Sheppard, Scott S.; Lacerda, Pedro; Ortiz, Jose L. (2008). "Photometric Lightcurves of Transneptunian Objects and Centaurs: Rotations, Shapes, and Densities". In M. Barucci, A.; Boehnhardt,H.; Cruikshank, D.P. and Morbidelli, A. (pdf). The Solar System Beyond Neptune. University of Arizona Press. pp. 129–142. ISBN 978-0-8165-2755-7. http://www.dtm.ciw.edu/users/sheppard/pub/SheppardKBOBook2008.pdf.
[edit] External links
- Orbital simulation from JPL (Java) / Ephemeris
- 37th DPS: Albedos, Diameters (and a Density) of Kuiper Belt and Centaur Objects
- Planet 10? Tiny 'Plutino' Almost Qualifies
- Discovery of a bright Trans-Neptunian Object (Yale)
- From the Rain Forest to Planet Huya
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