(82075) 2000 YW134
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(82075) 2000 YW134
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Discovery[1]
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| Discovered by | Kitt Peak |
| Discovery date | 2000-12-26 |
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Designations
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| MPC designation | (82075) 2000 YW134 |
| Minor planet category |
Scattered disc[2] Detached? 8:3 resonance?[3] |
| Epoch June 18, 2009 (2455000.5) | |
| Aphelion | 74.027 AU (Q) |
| Perihelion | 41.070 AU (q) |
| Semi-major axis | 57.548 AU (a) |
| Eccentricity | 0.31636 |
| Orbital period | 436.58 yr |
| Mean anomaly | 25.589° (M) |
| Inclination | 19.850° |
| Longitude of ascending node | 126.96° |
| Argument of perihelion | 315.51° |
| Satellites | S/2005 (82075) 1[4] (~237 km in diameter) |
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Physical characteristics
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| Dimensions | ~431 km (assumed)[5] <500 km[6] |
| Albedo | 0.09 (assumed)[5] >0.08[6] |
| Spectral type | B-V=0.92; V-R=0.55[7] |
| Apparent magnitude | ~21.4[8] |
| Absolute magnitude (H) | 4.74[7] |
(82075) 2000 YW134, provisionally known as 2000 YW134, is a binary trans-Neptunian object (TNO). It is classified as a scattered disc object and, possibly, a detached object.
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Contents
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Physical characteristics
Assuming a generic TNO albedo of 0.09, the primary is about 431 km in diameter and the secondary 237 km in diameter.[4][5] In 2010 2000 YW134 was observed by the Herschel Space Telescope in the far-infrared. No thermal radiation has been detected, which allowed astronomers to place an a upper limit on its size—the object (assuming it is singular) should be less than 500 km in diameter.[6]
In the visible the surface of 2000 YW134 is moderately red.[7]
Classifications
Dwarf planet?
With a generically estimated diameter of 431 km, 2000 YW134 is near the lower limit for the minimum size of a dwarf-planet candidate.[9] But as a dwarf-planet candidate, the large moon could give the binary system a double planet appearance when viewed from a distance.
Detached object?
2000 YW134 currently has a perihelion (q) distance of 41 AU.[1] Lykawka (2006) using a 4–5 Gyr integration seems to show 2000 YW134 as a detached object (with perihelion (q) > 40 AU). The Deep Ecliptic Survey (DES) using a 10My integration (last observation: 2007-11-10) shows it in a 8:3 resonance with a minimum perihelion (qmin) distance of 38.1 AU.[3] Emel’yanenko and Kiseleva in 2007 show a 84% chance that it is in the 8:3 resonance.[10]
Satellite
The moon of 2000 YW134 is relatively large compared to the primary, because the moon is only 1.3 magnitudes fainter than the primary.[11]
References
- ^ a b c "JPL Small-Body Database Browser: 82075 (2000 YW134)". 2007-11-10 last obs. http://ssd.jpl.nasa.gov/sbdb.cgi?sstr=82075. Retrieved 2009-10-06.
- ^ "List Of Centaurs and Scattered-Disk Objects". Minor Planet Center. http://www.minorplanetcenter.org/iau/lists/Centaurs.html. Retrieved 2009-10-07.
- ^ a b Marc W. Buie (2007-11-10 using 69 of 70 observations). "Orbit Fit and Astrometric record for 82075". SwRI (Space Science Department). http://www.boulder.swri.edu/~buie/kbo/astrom/82075.html. Retrieved 2009-10-06.
- ^ a b Wm. Robert Johnston (2006-03-04). "(82075) 2000 YW134". Johnston's Archive. http://www.johnstonsarchive.net/astro/astmoons/am-82075.html. Retrieved 2009-10-07.
- ^ a b c Wm. Robert Johnston (22 August 2008). "List of Known Trans-Neptunian Objects". Johnston's Archive. http://www.johnstonsarchive.net/astro/tnoslist.html. Retrieved 2009-10-06.
- ^ a b c Muller, T.G.; Lellouch, E.; Stansberry, J. et al. (2010). ""TNOs are Cool": A survey of the trans-Neptunian region I. Results from the Herschel science demonstration phase (SDP)". Astronomy and Astrophysics 518: L146. Bibcode 2010A&A...518L.146M. doi:10.1051/0004-6361/201014683.
- ^ a b c Stephen C. Tegler. "Kuiper Belt Object Magnitudes and Surface Color". Archived from the original on 05 June 2010. http://web.archive.org/web/20100605071153/http://www.physics.nau.edu/%7Etegler/research/survey.htm. Retrieved August 1, 2010.
- ^ "AstDys (82075) 2000YW134 Ephemerides". Department of Mathematics, University of Pisa, Italy. http://hamilton.dm.unipi.it/astdys/index.php?pc=1.1.3.0&n=82075. Retrieved 2009-10-06.
- ^ Mike Brown. "The Dwarf Planets". http://web.gps.caltech.edu/~mbrown/dwarfplanets. Retrieved 2009-10-07.
- ^ Emel’yanenko, V. V; Kiseleva, E. L. (2008). "Resonant motion of trans-Neptunian objects in high-eccentricity orbits". Astronomy Letters 34 (4): 271–279. Bibcode 2008AstL...34..271E. doi:10.1134/S1063773708040075.
- ^ Stephens, Denise C.; Noll, Keith S. (2006). "Detection of Six Transneptunian Binaries with NICMOS: A High Fraction of Binaries in the Cold Classical Disk". Astronomical Journal 131 (2): 1142–1148. arXiv:astro-ph/0510130. Bibcode 2006AJ....131.1142S. doi:10.1086/498715.
External links
- Orbital simulation from JPL (Java) / Horizons Ephemeris
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