2004 XR 190
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Asteroid 2004 XR 190 |
|
|---|---|
| Properties of the orbit ( animation ) | |
| Orbit type | DO, SDO , "Distant Object" |
| Major semi-axis | 57.255 AU |
| eccentricity | 0.107 |
| Perihelion - aphelion | 51.11 AU - 63.4 AU |
| Inclination of the orbit plane | 46.8 ° |
| Length of the ascending node | 252.4 ° |
| Argument of the periapsis | 285.5 ° |
| Time of passage of the perihelion | February 22, 2119 |
| Sidereal period | 433.24 a 2.9 M. |
| Mean orbital velocity | 3.904 km / s |
| Physical Properties | |
| Medium diameter | approx. 561 km |
| Albedo | 0.09 |
| Absolute brightness | 4.47 mag |
| history | |
| Explorer | Rhiannon Lynne Jones |
| Date of discovery | December 11, 2004 |
| Another name | "Buffy" |
| Source: Unless otherwise stated, the data comes from JPL Small-Body Database Browser . The affiliation to an asteroid family is automatically determined from the AstDyS-2 database . Please also note the note on asteroid items. | |
2004 XR 190 is a Trans- Neptunian object that is classified as a scattered disk object or a detached object in terms of its path dynamics . Because of its size, the asteroid is a dwarf planet candidate .
discovery
2004 XR 190 was discovered on December 11, 2004 by a team of astronomers led by Rhiannon Lynne Jones (Lynne Allen) of the University of British Columbia in Vancouver , Canada at the Mauna Kea Observatory ( Hawaii ). The team also included John J. Kavelaars , Brett Gladman , Jean-Marc Petit, Joel W. Parker, and Philip D. Nicholson. The discovery was announced on December 12, 2005.
Due to the amazing and difficult to explain property of a strongly tilted but almost circular orbit, the discovery team temporarily named the planetoid after the film character " Buffy " and sent further Inuit- based name suggestions to the International Astronomical Union (IAU). A name confirmation is currently pending.
After its discovery, HA 200 could be identified in photos up to December 6, 2002, which were taken at the Apache Point Observatory and found in the archive of the Sloan Digital Sky Survey , and thus its observation period was extended by two years to its Calculate orbit more accurately. In September 2018, a total of 139 observations were made over a period of 15 years. The last observation so far was carried out in September 2017 on the Pan-STARRS telescope. (As of February 9, 2019)
properties
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| Orbit from 2004 XR 190 (red) compared to the Kuiper belt . |
Orbit
2004 XR 190 orbits the sun in 433.24 years in an elliptical orbit between 51.11 AU and 63.40 AU from its center. The orbital eccentricity is 0.107, the orbit is inclined 46.79 ° with respect to the ecliptic . The planetoid is currently 42.62 AU from the Sun and 41.85 AU from Earth . In 1901 the planetoid reached its point furthest from the sun (aphelion). The next time it passes through perihelion in 2119, the last perihelion should have been in 1685.
The high inclination (orbit inclination) of 47 ° and the comparatively low orbit eccentricity are remarkable. The object was discovered because it happened to cross the plane of the ecliptic and was noticed when searching for distant objects in the solar system . This leads to the conclusion that there may be many more, as yet undiscovered objects with similar orbit parameters. The origin of this high inclination has not yet been clarified. 2004 XR 190 moves beyond the Kuiper Belt around the Sun, possibly an 8: 3 orbit resonance to Neptune . However, the orbital disturbances caused by the gravitational force of Neptune are minimal at such a distance that objects there should be in an orbit that has not changed since the formation of the solar system. 2004 XR 190 belongs to the same group as 2014 FC 72 , 2014 FZ 71 , 2015 FJ 345 and 2015 KQ 174 , all of which have poorly understood orbits with large perihelia and moderate eccentricities.
Marc Buie ( DES ) classifies the planetoid as an extended SDO (ESDO or DO ), while the Minor Planet Center classifies it as an SDO / Centaur and generally also as a "Distant Object" .
size
A diameter of around 561 km is currently assumed, based on a reflectivity of 9% and an absolute brightness of 4.6 m ; However, this is fraught with uncertainties, as the estimates range from 335 to 850 km due to the unknown albedo, which is assumed to be 0.04 to 0.25. The apparent magnitude of the 2004 XR 190 is 22.10 m . The mean surface temperature is estimated at 37 to 36 K (−236 to −237 ° C ) based on the distance from the sun .
Since it can be assumed that 2004 XR 190 is in hydrostatic equilibrium due to its size and must therefore be largely round, it should meet the criteria for classification as a dwarf planet . Mike Brown believes that the 2004 XR 190 is likely a dwarf planet. Gonzalo Tancredi made no recommendation in 2010.
| year | Dimensions km | source |
|---|---|---|
| 2008 | 529.0 | Tancredi |
| 2010 | 529.0 | Tancredi |
| 2018 | 612.0 | Johnston |
| 2018 | 561.0 | Brown |
| The most precise determination is marked in bold . | ||
| object |
q (AU) |
a (AU) |
T ( a ) |
e |
i (°) |
ω (°) |
H (likes) |
|---|---|---|---|---|---|---|---|
| 2012 VP 113 | 80.39 | 258.27 | 4.151 | 0.69 | 24.1 | 293.5 | 4.0 |
| (90377) Sedna | 76.26 | 484.52 | 10,665 | 0.84 | 11.9 | 311.4 | 1.3 |
| (541132) Leleākūhonua | 65.04 | 1031.49 | 33,128 | 0.94 | 11.7 | 118.0 | 5.5 |
| 2014 FZ 71 | 55.88 | 75.76 | 659 | 0.26 | 25.5 | 244.5 | 6.9 |
| 2015 RG 301 | 52.05 | 54.04 | 397 | 0.04 | 10.2 | 287.4 | 8.2 |
| 2014 FC 72 | 51.66 | 75.75 | 659 | 0.32 | 29.9 | 33.3 | 4.7 |
| 2018 GT 15 | 51.54 | 57.58 | 437 | 0.10 | 26.0 | 357.3 | 7.5 |
| 2004 XR 190 | 51.11 | 57.26 | 433 | 0.11 | 46.8 | 285.6 | 4.3 |
| 2015 FJ 345 | 50.69 | 62.88 | 499 | 0.19 | 35.0 | 77.4 | 7.9 |
| 2014 ST 373 | 50.19 | 104.56 | 1,069 | 0.52 | 43.2 | 297.1 | 5.4 |
| 2013 SY 99 | 50.02 | 693.86 | 18,277 | 0.93 | 4.2 | 32.1 | 6.7 |
| 2015 KQ 174 | 49.31 | 55.40 | 412 | 0.11 | 24.3 | 294.0 | 7.3 |
| 2010 GB 174 | 48.75 | 350.59 | 6,565 | 0.86 | 21.6 | 347.4 | 6.5 |
| 2014 SR 349 | 47.69 | 302.23 | 5,254 | 0.84 | 18.0 | 340.9 | 6.7 |
| (474640) 2004 VN 112 | 47.30 | 318.97 | 5,697 | 0.85 | 25.6 | 326.8 | 6.5 |
See also
- List of trans-Neptunian objects
- List of dwarf planets of the solar system
- List of asteroids
- List of moons from asteroids
Web links
- Path parameters
- Discovery website of the research team ( Memento of July 27, 2008 in the Internet Archive ) (English)
- Article in the New Scientist ( Memento of May 12, 2008 in the Internet Archive )
- How many dwarf planets are there in the outer solar system? Current list of the largest TNOs from Mike Brown
- Free the dwarf planets! Mike Brown's column on the IAU and the dwarf planets regarding their classifications (23 August 2011)
Individual evidence
- ^ A b Marc W. Buie : Orbit Fit and Astrometric record for 04XR190 . SwRI (Space Science Department). Retrieved February 9, 2019.
- ↑ a b MPC : MPEC List Of Centaurs and Scattered-Disk Objects . IAU . Retrieved February 9, 2019.
- ↑ a b c 2004 XR190 at the IAU Minor Planet Center (English). Accessed February 9, 2019.
- ↑ v ≈ π * a / period (1 + sqrt (1-e²))
- ↑ MPC : MPEC 2005-X72: 2004 XR190 . IAU . December 12, 2005. Retrieved February 9, 2019.
- ^ Maggie McKee: Strange new object found at the edge of the Solar System. In: New Scientist. December 13, 2005, accessed August 13, 2017 ( These traits make the object, nicknamed “Buffy” after the US television series about a vampire slayer, hard to explain. “Maybe Buffy is going to be a bit of a theory slayer” ).
- ↑ 2004 XR190 in the Small-Body Database of the Jet Propulsion Laboratory (English). Retrieved February 9, 2019.
- ^ E. Schaller, Mike Brown : Volatile Loss and Retention on Kuiper Belt Objects (PDF) . In: The Astronomical Journal . 659, No. 1, April 10, 2007, pp. L61-L64. bibcode : 2007ApJ ... 659L..61S . doi : 10.1086 / 516709 .
- ↑ RL Allen u. a .: Discovery of a Low-Eccentricity, High-Inclination Kuiper Belt Object at 58 AU (PDF) . In: The Astronomical Journal . 640, No. 1, December 16, 2005, pp. L83-L86. bibcode : 2006ApJ ... 640L..83A . doi : 10.1086 / 503098 .
- ↑ 2004 XR190 in the database of the "Asteroids - Dynamic Site" (AstDyS-2, English).
- ↑ a b Mike Brown : How many dwarf planets are there in the outer solar system? . CalTech . November 12, 2018. Retrieved February 9, 2019.
- ↑ a b Gonzalo Tancredi: Physical and dynamical characteristics of icy “dwarf planets” (plutoids) (PDF) . In: IAU (Ed.): Icy Bodies of the Solar System: Proceedings IAU Symposium No. 263, 2009 . 2010. doi : 10.1017 / S1743921310001717 . Retrieved February 9, 2019.
- ^ Gonzalo Tancredi, Sofía Favre: DPPH List . In: Dwarf Planets and Plutoid Headquarters, from Which are the dwarfs in the solar system? . August. Retrieved February 9, 2019.
- ^ Wm. R. Johnston: List of Known Trans-Neptunian Objects . Johnston's Archives. October 7, 2018. Retrieved February 9, 2019.
- ↑ List of objects with q> 47. Minor Planet Center (MPC) of the International Astronomical Union (IAU), accessed on June 13, 2020 .
- ↑ Chadwick A. Trujillo, Michael E. Brown: The Radial Distribution of the Kuiper Belt . In: The Astrophysical Journal Letters . Vol. 554, No. 1 , May 31, 2001, p. L95 , doi : 10.1086 / 320917 , bibcode : 2001ApJ ... 554L..95T (English).