(119951) 2002 KX ₁₄

Asteroid (119951) 2002 KX 14
Properties of the orbit ( animation ) Epoch:  April 27, 2019 ( JD 2,458,600.5)
Orbit type	CKBO  ( Cold ) Distant Object
Major semi-axis	39,086  AU
eccentricity	0.044
Perihelion - aphelion	37.356 AU - 40.816 AU
Inclination of the orbit plane	0.4 °
Length of the ascending node	287.2 °
Argument of the periapsis	63.6 °
Time of passage of the perihelion	August 4, 2077
Sidereal period	244 a 4.4 M
Mean orbital velocity	4.725 km / s
Physical Properties
Medium diameter	${\displaystyle 455_{-27}^{+27}\,\mathrm {km} }$
Albedo	${\displaystyle 0{,}097_{-0,013}^{+0,014}\mathrm {} }$
Absolute brightness	4.862 ± 0.038 mag
Spectral class	C B-V = 1.050 ± 0.030 VR = 0.610 ± 0.010 VI = 1.290 ± 0.014 BR = 1.660 ± 0.040
history
Explorer	Chadwick A. Trujillo Michael E. Brown
Date of discovery	May 17, 2002
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.

(119951) 2002 KX ₁₄ is a large trans-Neptunian object in the Kuiper belt , which is classified as Cubewano (CKBO) in terms of orbital dynamics . Because of its size, the asteroid is a dwarf planet candidate .

discovery

2002 KX ₁₄ was discovered on May 17, 2002 by a team of astronomers consisting of Chad Trujillo ( Gemini Observatory ) and Mike Brown ( CalTech ) as part of the Near Earth Asteroid Tracking Project (NEAT) at 1.2 m –Oschin Schmidt telescope discovered at Palomar Observatory ( California ). The discovery was announced on 23 April 2003, the asteroid was awarded in November 2005 by the IAU , the Minor Planet -number 119951 .

After its discovery, KX _{14 could be identified} in photos up to May 31, 1984, taken as part of the Digitized Sky Survey (DSS) program at the Siding Spring Observatory , and thus its observation period was extended by 18 years in order to calculate its orbit more precisely. Since then, the planetoid has been observed through various telescopes such as the Herschel and Spitzer space telescopes as well as earth-based telescopes. In April 2017, a total of 176 observations were made over a period of 32 years. The last observation so far was carried out in June 2015 on the Pan-STARRS telescope (PS1). (As of March 13, 2019)

properties

The orbit of 2002 KX ₁₄ (blue, light blue) compared to Pluto and the giant planets (white, gray).

Solar distance from 2002 KX ₁₄ and Pluto in a period of around 50,000 years.

Orbit

2002 KX ₁₄ orbits the sun in 244.37 years in an almost circular orbit between 37.36  AU and 40.82 AU from its center. The eccentricity of the orbit is 0.044, the orbit is hardly inclined with respect to the ecliptic at 0.40 ° . The planetoid is currently 39.05 AU from the Sun. He will next pass through perihelion in 2077, so the last perihelion should have occurred in 1833.

The semi-major axis , orbital period and eccentricity of 2002 KX ₁₄ are located near the Plutinos - which also includes Pluto - which usually have orbital periods of around 247.2 years, which is roughly 1.5 times the solar distance of the planet Neptune . However, since 2002 KX ₁₄ does not show a 2: 3 resonance with Neptune, it does not count among the Plutinos; these also mostly have much higher orbital inclinations, whereas 2002 KX ₁₄ orbits the sun almost perfectly on the ecliptic plane and its uniform orbit is therefore more similar to that of the planets. It is believed that the planetoid was formed on the orbit it is still on today.

Marc Buie ( DES ) classifies the planetoid as Cubewano , where he according to a simulation than 10 million years on the ground dynamically cold classic KBO heard; this has nothing to do with the temperature, but means that the planetoid has not experienced any significant orbital disturbances from Neptune since its formation . The Minor Planet Center does not have a specific classification, it classifies it as a non-SDO and generally as a distant object .

size

A diameter of 455 km is currently assumed, based on a reflectivity of 9.7% and an absolute brightness of 4.86  ^m , which was determined using data from the Spitzer and Herschel space telescopes. Assuming a diameter of 455 km, this results in a total surface of around 650,000 km². The apparent brightness of 2002 KX ₁₄ is 20.82 ^m , the mean surface temperature is estimated at 43 K (−230 ° C) based on the distance from  the sun  .

Since it can be assumed that 2002 KX ₁₄ 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 2002 KX ₁₄ may be a dwarf planet. Gonzalo Tancredi did not make a recommendation in 2010.

Determination of the diameter for 2002 KX ₁₄

year	Dimensions km	source
2008	<561.6 +219.9−181.5	Stansberry et al. a.
2008	<440.0 180.0 +50.0−38.0	Brucker et al. a.
2008	554.0	Tancredi
2010	554.0	Tancredi
2012	455.0 ± 27.0	Vilenius et al. a.
2012	482.53	LightCurve DataBase
2012	> 414.0 ± 4.0	Alvarez-Candal et al. a.
2014	> 365.0 +30.0−21.0	Alvarez-Candal et al. a.
2018	468.0	Brown
The most precise determination is marked in bold .

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

• Precovery photos of 2002 KX ₁₄
• 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

1. ^ ^{A b} Marc W. Buie : Orbit Fit and Astrometric record for 119951 . SwRI (Space Science Department). Retrieved March 8, 2019.
2. ↑ E. Lellouch et al. a .: “TNOs are Cool”: A survey of the trans-Neptunian region. IX. Thermal properties of Kuiper belt objects and Centaurs from combined Herschel and Spitzer observations (PDF) . In: Astronomy and Astrophysics . 557, No. A60, June 10, 2013, p. 19. bibcode : 2013A & A ... 557A..60L . doi : 10.1051 / 0004-6361 / 201322047 .
3. ^ ^{A b} Wm. R. Johnston: List of Known Trans-Neptunian Objects . Johnston's Archives. October 7, 2018. Retrieved March 8, 2019.
4. ↑ ^{a b c} (119951) 2002 KX14 at IAU Minor Planet Center (English) Retrieved March 8, 2019.
5. ↑ v ≈ π * a / period (1 + sqrt (1-e²))
6. ↑ ^{a b c d} E. Vilenius u. a .: “TNOs are Cool”: A survey of the trans-Neptunian region VI. Herschel / PACS observations and thermal modeling of 19 classical Kuiper belt objects (PDF) . In: Astronomy and Astrophysics . 541, No. A94, April 4, 2012, p. 17. arxiv : 1204.0697 . bibcode : 2012A & A ... 541A..94V . doi : 10.1051 / 0004-6361 / 201118743 .
7. ↑ ^{a b} LCDB Data for (119951) 2002KX14 . MinorPlanetInfo. 2016. Accessed March 8, 2019.
8. ↑ ^{a b} S. Tegler u. a .: Two Color Populations of Kuiper Belt and Centaur Objects and the Smaller Orbital Inclinations of Red Centaur Objects (PDF) . In: The Astronomical Journal . 152, No. 6, December 2016, p. 210, 13. bibcode : 2016AJ .... 152..210T . doi : 10.3847 / 0004-6256 / 152/6/210 .
9. ↑ ^{a b} H. Boehnhardt u. a .: Photometry of Transneptunian Objects for the Herschel Key Program “TNOs are Cool” . In: Earth, Moon, and Planets . 114, No. 1-2, November 2014, pp. 35-57. bibcode : 2014EM & P..114 ... 35B . doi : 10.1007 / s11038-014-9450-x .
10. ↑ MPC : MPEC 2003-H13: 2002 KX14 . IAU . April 23, 2003. Retrieved March 8, 2019.
11. ↑ MPC : MPC / MPO / MPS Archive . IAU . Retrieved March 8, 2019.
12. ↑ (119951) 2002 KX14 in the Small-Body Database of the Jet Propulsion Laboratory (English). Retrieved March 8, 2019.
13. ↑ MPC : MPEC 2010-S44: Distant Minor Planets (2010 OCT.11.0 TT) . IAU . September 25, 2010. Retrieved March 8, 2019.
14. ↑ MPC : MPEC List Of Centaurs and Scattered-Disk Objects . IAU . Retrieved March 8, 2019.
15. ↑ (119951) 2002 KX14 in the database of the "Asteroids - Dynamic Site" (AstDyS-2, English).
16. ↑ ^{a b} Mike Brown : How many dwarf planets are there in the outer solar system? . CalTech . November 12, 2018. Retrieved March 8, 2019.
17. ^ ^{A b} G. Tancredi: Physical and dynamical characteristics of icy “dwarf planets” (plutoids) (PDF) . In: International Astronomical Union (Ed.): Icy Bodies of the Solar System: Proceedings IAU Symposium No. 263, 2009 . 2010. doi : 10.1017 / S1743921310001717 . Retrieved March 8, 2019.
18. ↑ J. Stansberry et al. a .: Physical Properties of Kuiper Belt and Centaur Objects: Constraints from Spitzer Space Telescope (PDF) . In: University of Arizona Press . 592, No. 161-179, February 20, 2007. arxiv : astro-ph / 0702538 . bibcode : 2008ssbn.book..161S .
19. ↑ M. Brucker et al. a .: High Albedos of Low Inclination Classical Kuiper Belt Objects (PDF) . In: Icarus . 201, No. 1, December 18, 2008. arxiv : 0812.4290 . bibcode : 2009Icar..201..284B . doi : 10.1016 / j.icarus.2008.12.040 .
20. ^ G. Tancredi, S. Favre: DPPH List . In: Dwarf Planets and Plutoid Headquarters, from Which are the dwarfs in the solar system? . September. Retrieved March 8, 2019.
21. ↑ A. Alvarez-Candal et al. a .: Stellar occultation by the trans-Neptunian object 2002 KX ₁₄ (PDF) . In: European Planetary Science Congress 2012 . EPSC2012-482, September 28, 2012. bibcode : 2012epsc.conf..482A .
22. ↑ A. Alvarez-Candal et al. a .: Stellar occultation by (119951) 2002 KX ₁₄ on April 26, 2012 . In: Astronomy and Astrophysics . 571, No. A48, November 2014, p. 8. bibcode : 2014A & A ... 571A..48A . doi : 10.1051 / 0004-6361 / 201424648 .