(445473) 2010 VZ98: Difference between revisions
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Revision as of 18:56, 9 September 2016
| Discovery [1][2] | |
|---|---|
| Discovered by | D. L. Rabinowitz M. E. Schwamb S. Tourtellotte |
| Discovery site | La Silla Obs. |
| Discovery date | 11 November 2010 |
| Designations | |
| (445473) 2010 VZ98 | |
| 2010 VZ98 | |
| TNO[3] · SDO[4] | |
| Orbital characteristics [3] | |
| Epoch 31 July 2016 (JD 2457600.5) | |
| Uncertainty parameter 2 | |
| Observation arc | 16.90 yr (6,171 days) |
| Aphelion | 269.36 AU |
| Perihelion | 34.323 AU |
| 151.84 AU | |
| Eccentricity | 0.7740 |
| 1871.06 yr (683,405 days) | |
| 357.81° | |
| 0° 0m 1.8s / day | |
| Inclination | 4.5099° |
| 117.43° | |
| 313.91° | |
| Physical characteristics | |
| Dimensions | 401.33 km (calculated)[5] 461 km (assumed)[6] |
| 9.72±0.05 h[5][7] | |
| 0.07 (assumed)[6] 0.10 (assumed)[5] | |
| C [5] | |
| 4.81±0.04 (S)[7] 5.1[3][5] | |
(445473) 2010 VZ98 is a trans-Neptunian object (TNO) orbiting the Sun in the scattered disc. It was discovered on 11 November 2010, by American astronomers David L. Rabinowitz, Megan E. Schwamb and Suzanne W. Tourtellotte at La Silla in northern Chile,[2] when it was 38 AU from the Sun. With an absolute magnitude of approximately 5.0 and a calculated diameter above 400 kilometers, it is possibly a dwarf planet.[6]
The carbonaceous TNO orbits the Sun at a distance of 34.3–269.4 AU once every 1871 years and 1 month (683,405 days). Its orbit has a high eccentricity of 0.77 and an inclination of 5° with respect to the ecliptic.[3] Small number statistics suggest that this body may be trapped in a 3:2 orbital resonance with an unseen planet beyond Neptune with a semi-major axis of 195–215 AU.[8] The first precovery was taken by the Sloan Digital Sky Survey at the Apache Point Observatory in 1998, extending the body's observation arc by 12 years prior to its discovery. The precoveries were found in May 2015 (MPS 604632).[2]
Published in 2013, a rotational light-curve was obtained for this object from photometric observation by members of the Carnegie Institution for Science at Las Campanas Observatory, Chile. The light-curve gave a rotation period of 9.72±0.05 hours with a brightness variation of 0.18 magnitude (U=n.a.).[7] While American astronomer Michael E. Brown assumes a diameter of 461 kilometers and an albedo of 0.07,[6] the Collaborative Asteroid Lightcurve Link assumes an albedo of 0.10 and calculates a diameter of 401 kilometers.[5]
See also
References
- ^ "MPEC 2011-Q57 : 2010 VZ98". IAU Minor Planet Center. 2011-08-31. Retrieved 2012-08-31.
- ^ a b c "445473 (2010 VZ98)". Minor Planet Center. Retrieved 7 September 2016.
- ^ a b c d "JPL Small-Body Database Browser: 445473 (2010 VZ98)" (2015-10-12 last obs.). Jet Propulsion Laboratory. Retrieved 7 September 2016.
- ^ "List Of Centaurs and Scattered-Disk Objects". Minor Planet Center. Retrieved 2012-08-31.
- ^ a b c d e f "LCDB Data for (445473)". Asteroid Lightcurve Database (LCDB). Retrieved 7 September 2016.
- ^ a b c d Michael E. Brown. "How many dwarf planets are there in the outer solar system?". California Institute of Technology. Retrieved 7 September 2016.
- ^ a b c Benecchi, Susan D.; Sheppard, Scott S. (May 2013). "Light Curves of 32 Large Transneptunian Objects" (PDF). The Astronomical Journal. 145 (5): 19. arXiv:1301.5791. Bibcode:2013AJ....145..124B. doi:10.1088/0004-6256/145/5/124. Retrieved 7 September 2016.
- ^ de la Fuente Marcos, C.; de la Fuente Marcos, R. (September 2014). "Extreme trans-Neptunian objects and the Kozai mechanism: signalling the presence of trans-Plutonian planets". Monthly Notices of the Royal Astronomical Society: Letters. 443 (1): L59–L63. arXiv:1406.0715. Bibcode:2014MNRAS.443L..59D. doi:10.1093/mnrasl/slu084. Retrieved 7 September 2016.
