(144897) 2004 UX ₁₀

Asteroid (144897) 2004 UX 10
Properties of the orbit ( animation ) Epoch:  April 27, 2019 ( JD 2,458,600.5)
Orbit type	CKBO  ("Hot") "Distant Object"
Major semi-axis	38.871  AU
eccentricity	0.044
Perihelion - aphelion	37,152 AU - 40,591 AU
Inclination of the orbit plane	9.5 °
Length of the ascending node	147.9 °
Argument of the periapsis	149.2 °
Time of passage of the perihelion	June 24, 1950
Sidereal period	242 a 4.2 M
Mean orbital velocity	4.738 km / s
Physical Properties
Medium diameter	${\displaystyle 398{,}1_{-39,3}^{+32,6}\,\mathrm {km} }$
Albedo	${\displaystyle 0{,}141_{-0,031}^{+0,044}\mathrm {} }$
Medium density	> 1.21 g / cm³
Rotation period	5.68 ± 0.05 h (0.237 d )
Absolute brightness	4.75 ± 0.16 mag
Spectral class	C B-V = 0.950 ± 0.020 VR = 0.580 ± 0.030 BR = 1.530 ± 0.020
history
Explorer	Andrew C. Becker Andrew W. Puckett Jeremy M. Kubica
Date of discovery	October 20, 2004
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.

(144897) 2004 UX ₁₀ is a large trans-Neptunian object in the Kuiper belt , which is classified as Cubewano (CKBO) in terms of railway dynamics . Due to its size, the asteroid may be one of the dwarf planet candidates .

discovery

2004 UX ₁₀ was on 20 October 2004 by a team of astronomers consisting of Andrew Becker, Andrew Puckett and Jeremy Martin Kubica, with the 2.5-m Ritchey Chretien telescope at Apache Point Observatory ( New Mexico discovered). The discovery was announced on 21 August 2006, the asteroid was on 5 December 2006 by the IAU , the Minor Planet -number 144897 .

After its discovery, UX _{10 could be identified} in photos up to August 15, 1953, taken as part of the Digitized Sky Survey (DSS) program at the Palomar Observatory ( California ), and thus its observation period by 51 years to calculate its orbit more precisely. Since then, the asteroid has been observed through various telescopes such as the Herschel Space Telescope and Earth-based telescopes. In October 2018, a total of 230 observations over a period of 66 years were available. The last observation so far was carried out at the Purple Mountain Observatory in October 2018 . (As of March 9, 2019)

properties

Orbit

2004 UX ₁₀ orbits the sun in 242.35 years in an almost circular orbit between 37.15  AU and 40.59 AU from its center. The eccentricity of the orbit is 0.044, the orbit is inclined at 9.53 ° to the ecliptic . The planetoid is currently 39.30 AU from the sun. He last passed through perihelion in 1950, so the next perihelion should take place in 2192.

Marc Buie ( DES ) classifies the planetoid as Cubewano , where he to the ground dynamically hot classical KBO heard during the Minor Planet Center is no specific classification, it assigns it as a non-SDO and commonly referred to as Distant Object one.

Size and rotation

A diameter of 398.1 km is currently assumed, based on a reflectivity of 14.1% and an absolute brightness of 4.75  ^m , which was determined using data from the Herschel space telescope. Assuming a diameter of 398 km, the total surface area is around 498,000 km ² . The apparent magnitude of 2004 UX ₁₀ is 20.58  ^m .

Since it is conceivable that 2004 UX ₁₀ is in hydrostatic equilibrium due to its size and could therefore be largely round, it may meet the criteria for classification as a dwarf planet . Mike Brown , who estimates the diameter itself at 409 km ( albedo 14%, absolute brightness 4.8  ^m ), assumes that 2004 UX _{10 is} possibly a dwarf planet. Gonzalo Tancredi did not make a recommendation in 2010.

Using light curve observations , the 2004 UX ₁₀ rotates once around its axis in 5 hours and 40.8 minutes. This means that in a 2004 UX ₁₀ year it performs 374027.2 self- rotations (“days”). However, this is still fraught with uncertainties, as the observation time at that time was insufficient and the error rate is around 30%.

The asteroid has a reddish color in the visible spectrum ; it shows no surface characteristics, but there is a small deviation in the absorption lines at 0.8 μm.

Determinations of the diameter for 2004 UX ₁₀

year	Dimensions km	source
2008	505.0	Tancredi
2010	529.0	Tancredi
2012	398.1 +32.6−39.3	Mommert et al. a.
2012	554.02	LightCurve DataBase
2018	409.0	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 from 2004 UX ₁₀
• 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 144897 . SwRI (Space Science Department). Retrieved March 9, 2019.
2. ^ ^{A b} Wm. R. Johnston: List of Known Trans-Neptunian Objects . Johnston's Archives. October 7, 2018. Retrieved March 9, 2019.
3. ↑ ^{a b c} (144897) 2004 UX10 at IAU Minor Planet Center (English) Retrieved March 9, 2019.
4. ↑ v ≈ π * a / period (1 + sqrt (1-e²))
5. ↑ ^{a b c d} M. Mommert u. a .: “TNOs are Cool”: A survey of the trans-Neptunian region. V. Physical characterization of 18 Plutinos using Herschel-PACS observations (PDF) . In: Astronomy and Astrophysics . 541, no.A93 , February 16, 2012. arxiv : 1202.3657 . bibcode : 2012A & A ... 541A..93M . doi : 10.1051 / 0004-6361 / 201118562 .
6. ↑ ^{a b} A. Thirouin et al. a .: Short-term variability of a sample of 29 trans-Neptunian objects and Centaurs . In: Astronomy and Astrophysics . 522, No. A93, April 27, 2010, p. 43. arxiv : 1004.4841 . bibcode : 2010A & A ... 522A..93T . doi : 10.1051 / 0004-6361 / 200912340 .
7. ↑ ^{a b} LCDB Data for (144897) 2004UX10 . MinorPlanetInfo. 2016. Accessed March 9, 2019.
8. ↑ ^{a b} O. Hainaut u. a .: Colors of minor bodies in the outer solar system. II. A statistical analysis revisited (PDF) . In: Astronomy and Astrophysics . 546, No. A115, September 10, 2012, p. 20. arxiv : 1209.1896 . bibcode : 2012A & A ... 546A.115H . doi : 10.1051 / 0004-6361 / 201219566 .
9. ↑ N. Peixinho et al. a .: The bimodal colors of Centaurs and small Kuiper belt objects (PDF) . In: Astronomy and Astrophysics . 546, No. A86, June 14, 2012, p. 12. arxiv : 1206.3153 . bibcode : 2012A & A ... 546A..86P . doi : 10.1051 / 0004-6361 / 201219057 .
10. ↑ MPC : MPEC 2006-Q16: 2004 UX10 . IAU . August 21, 2006. Retrieved March 9, 2019.
11. ↑ MPC : MPC / MPO / MPS Archive . IAU . Retrieved March 9, 2019. Reference there: MPC 58201 (PDF)
12. ↑ (144897) 2004 UX10 in the Small-Body Database of the Jet Propulsion Laboratory (English). Retrieved March 9, 2019.
13. ↑ MPC : MPEC 2010-S44: Distant Minor Planets (2010 OCT.11.0 TT) . IAU . September 25, 2010. Retrieved March 9, 2019.
14. ↑ MPC : MPEC List Of Centaurs and Scattered-Disk Objects . IAU . Retrieved March 9, 2019.
15. ↑ (144897) 2004 UX10 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 9, 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 9, 2019.
18. ↑ S. Fornasier et al. a .: Visible spectroscopy of the new ESO large programs on trans-Neptunian objects and Centaurs: final results (PDF) . In: Astronomy and Astrophysics . 508, No. 1, December 2009, pp. 457-465. arxiv : 0910.0450 . bibcode : 2009A & A ... 508..457F . doi : 10.1051 / 0004-6361 / 200912582 .
19. ^ G. Tancredi, S. Favre: DPPH List . In: Dwarf Planets and Plutoid Headquarters, from Which are the dwarfs in the solar system? . September. Retrieved March 9, 2019.