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2012 VP113
Discovery images taken on November 5, 2012. A merger of three discovery images, the red, green and blue dots on the image represent 2012 VP113's location on each of the images, taken two hours apart from each other.
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| Discovery[1] | |
|---|---|
| Discovered by | Scott Sheppard Chad Trujillo Cerro Tololo Inter-American Observatory (807) |
| Discovery date | 5 November 2012 announced: 26 March 2014 |
| Designations | |
| MPC designation | 2012 VP113 |
| TNO, sednoid | |
| Orbital characteristics[3] | |
| Epoch JD 2457000.5 (9 December 2014) (Uncertainty=5) |
|
| Observation arc | 2.02 years |
| Aphelion | 446 ± 13 AU (Q) |
| Perihelion | 80.5 ± 0.6 AU (q) |
| 263 ± 7 AU (a) | |
| Eccentricity | 0.696 ± 0.011 |
| 4268 ± 179 yr 4300 yr (barycentric)[2] |
|
| 3.0±0.2 | |
| Inclination | 24.024°±0.004° |
| 90.87°±0.01° (Ω) | |
| 294°±2° (ω) | |
| Physical characteristics | |
| Dimensions | 300–1000 km[4] 450 km (assumed)[4][5] 600 km[6] |
| Albedo | 0.15 (Nature; 2014)[5] 0.1 (Brown website)[6] |
|
Spectral type
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(moderately red) V−R = 0.52 ± 0.04[5] B−V = 0.92 |
| 23.4 | |
| 4.0 (MPC)[7] 4.0 (JPL)[3] 4.3 [6] |
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2012 VP113 is a planetoid in the outer reaches of the Solar System. It is the object with the farthest known perihelion (closest approach to the Sun) in the Solar System, farther than Sedna's.[8] Its discovery was announced on 26 March 2014.[5][9] It has an absolute magnitude (H) of 4.0,[7] which makes it likely to be a dwarf planet,[6] and it is accepted as a dwarf planet by some.[10] It is expected to be about half the size of Sedna and similar in size to Huya.[4] The similarity of 2012 VP113's orbit to the orbits of other known extreme trans-Neptunian objects led Scott Sheppard and Chad Trujillo to suggest that an undiscovered super-Earth in the outer Solar System is shepherding these distant objects into similar type orbits.[5]
Its surface is thought to have a pink tinge, resulting from chemical changes produced by the effect of radiation on frozen water, methane, and carbon dioxide.[11] This optical color is consistent with formation in the gas-giant region and not the classical Kuiper belt, which is dominated by ultra-red colored objects.[5]
Contents
History[edit]
Discovery[edit]
2012 VP113 was first observed on 5 November 2012[1] with NOAO's 4-meter Víctor M. Blanco Telescope at the Cerro Tololo Inter-American Observatory.[12] Carnegie’s 6.5-meter Magellan telescope at Las Campanas Observatory in Chile was used to determine its orbit and surface properties.[12] Before being announced to the public, it was only tracked by Cerro Tololo Inter-American Observatory (807) and Las Campanas Observatory (304).[7] It has an observation arc of about 2 years.[3] Two precovery measurements from 22 October 2011 have been reported.[7] A primary issue with observing it and finding precovery observations of it is that at an apparent magnitude of 23, it is too faint for most telescopes to easily observe.
Nickname[edit]
2012 VP113 was abbreviated "VP" and nicknamed "Biden" by the discovery team, after Joe Biden, the Vice President (VP) of the United States.[9]
Orbit[edit]
2012 VP113 has the largest perihelion distance of any known object in the Solar System.[13] Its last perihelion was around 1979,[a] at a distance of 80 AU;[3] it is currently 83 AU from the Sun. Only four other Solar System objects are known to have perihelia larger than 47 AU: Sedna (76 AU), 2004 XR190 (51 AU), 2010 GB174 (48 AU), and 2004 VN112 (47 AU).[13] The paucity of bodies with perihelia at 50–75 AU appears not to be an observational artifact.[5]
It is possibly a member of a hypothesized Hills cloud.[4][12][14] It has a perihelion, argument of perihelion, and current position in the sky similar to those of Sedna.[4] In fact, all known Solar System bodies with semi-major axes over 150 AU and perihelia greater than Neptune's have arguments of perihelion clustered near 340 ± 55°.[5] This could indicate a similar formation mechanism for these bodies.[5] (148209) 2000 CR105 was the first such object discovered.
It is currently unknown how 2012 VP113 acquired a perihelion distance beyond the Kuiper belt. The characteristics of its orbit, like those of Sedna's, have been explained as possibly created by a passing star or a trans-Neptunian planet of several Earth masses hundreds of astronomical units from the Sun.[15] The orbital architecture of the trans-Plutonian region may signal the presence of more than one planet.[16][17] 2012 VP113 could even be captured from another planetary system.[10] However, it is considered more likely that the perihelion of 2012 VP113 was raised by multiple interactions within the crowded confines of the open star cluster in which the Sun formed.[4]
| Object name | Distance from the Sun (AU) | Magnitude (vmag) |
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| Current | Perihelion | Aphelion | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| V774104 | 103 | N/A | N/A | 24 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Eris | 96.3 | 37.8 | 97.6 | 18.7 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| 2007 OR10 | 87.5 | 33.0 | 100.8 | 21.7 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Sedna | 85.7 | 76.0 | 939 | 21.0 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| 2014 FC69 | 84.2 | 40.3 | 106.9 | 24.1 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| 2006 QH181 | 83.4 | 37.8 | 96.7 | 23.6 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| 2012 VP113 | 83.3 | 80.5 | 438 | 23.4 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| 2013 FY27 | 80.3 | 36.1 | 81.8 | 22.1 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| 2010 GB174 | 70.8 | 48.7 | 693 | 25.1 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| 2000 CR105 | 60.5 | 44.3 | 412 | 23.9 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| 2008 ST291 | 59.9 | 42.4 | 154.5 | 22.2 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| 2003 QX113 | 59.9 | 36.7 | 62.1 | 22.5 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Including all known objects currently located at least twice as far as Neptune.[18] See List of trans-Neptunian objects for more. |
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Comparison[edit]
See also[edit]
- List of Solar System objects most distant from the Sun in 2015
- V774104
- 90377 Sedna (relatively large and also distant body)
- List of hyperbolic comets
- Pluto
- Have very large aphelion
Notes[edit]
- ^ The 1-sigma uncertainty in the year of perihelion passage is ~4 years using JPL solution 2.[3]
References[edit]
- ^ a b "MPEC 2014-F40 : 2012 VP113". IAU Minor Planet Center. 2014-03-26. Retrieved 2014-03-26. (K12VB3P)
- ^ Horizons output. "Barycentric Osculating Orbital Elements for 2012 VP113". Retrieved 2016-01-23. (Ephemeris Type:Elements and Center:@0)
- ^ a b c d e "JPL Small-Body Database Browser: (2012 VP113)" (last observation: 2013-10-30 (arc=~2 year)). Jet Propulsion Laboratory. Retrieved 2014-03-31.
- ^ a b c d e f Lakdawalla, Emily (2014-03-26). "A second Sedna! What does it mean?". Planetary Society blogs. The Planetary Society. Retrieved 2014-03-27.
- ^ a b c d e f g h i Trujillo, C. A.; Sheppard, S. S. (2014). "A Sedna-like body with a perihelion of 80 astronomical units" (PDF). Nature 507 (7493): 471–474. Bibcode:2014Natur.507..471T. doi:10.1038/nature13156. Archived (PDF) from the original on 2014-12-16.
- ^ a b c d Brown, Michael E. (2014-04-17). "How many dwarf planets are there in the outer solar system? (updates daily)". California Institute of Technology. Retrieved 2014-04-17.
- ^ a b c d "2012 VP113 Orbit" (arc=739 days over 3 oppositions). IAU Minor Planet Center. Retrieved 2014-03-26.
- ^ Chang, Kenneth (2014-03-26). "A New Planetoid Reported in Far Reaches of Solar System". New York Times. Retrieved 2014-03-26.
- ^ a b Witze, Alexandra (2014-03-26). "Dwarf planet stretches Solar System's edge". Nature. doi:10.1038/nature.2014.14921.
- ^ a b Sheppard, Scott S. "Beyond the Edge of the Solar System: The Inner Oort Cloud Population". Department of Terrestrial Magnetism, Carnegie Institution for Science. Retrieved 2014-03-27.
- ^ Sample, Ian (2014-03-26). "Dwarf planet discovery hints at a hidden Super Earth in solar system". The Guardian. Retrieved 2014-03-27.
- ^ a b c "NASA Supported Research Helps Redefine Solar System's Edge". NASA. 2014-03-26. Retrieved 2014-03-26.
- ^ a b "JPL Small-Body Database Search Engine: q > 47 (AU)". JPL Solar System Dynamics. Retrieved 2014-03-26.
- ^ Wall, Mike (2014-03-26). "New Dwarf Planet Found at Solar System's Edge, Hints at Possible Faraway 'Planet X'". Space.com web site. TechMediaNetwork. Retrieved 2014-03-27.
- ^ "A new object at the edge of our Solar System discovered". Physorg.com. 2014-03-26.
- ^ de la Fuente Marcos, Carlos; de la Fuente Marcos, Raúl (1 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.
- ^ de la Fuente Marcos, Carlos; de la Fuente Marcos, Raúl; Aarseth, S. J. (11 January 2015). "Flipping minor bodies: what comet 96P/Machholz 1 can tell us about the orbital evolution of extreme trans-Neptunian objects and the production of near-Earth objects on retrograde orbits". Monthly Notices of the Royal Astronomical Society 446 (2): 1867–1873. arXiv:1410.6307. Bibcode:2015MNRAS.446.1867D. doi:10.1093/mnras/stu2230.
- ^ a b "AstDyS-2, Asteroids - Dynamic Site". 2016-02-26. Retrieved 2016-02-29.
Objects with distance from Sun over 59 AU
External links[edit]
Media related to 2012 VP113 at Wikimedia Commons
- Orbital simulation from JPL (Java) / Horizons Ephemeris
- 2012 VP113 Inner Oort Cloud Object Discovery Images from Scott S. Sheppard/Carnegie Institution for Science.
- 2012 VP113 has Q=460 ± 30 (mpml: CFHT 2011-Oct-22 precovery)
- 2012 VP113 at the JPL Small-Body Database
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