# (202421) 2005 UQ 513

Asteroid
(202421) 2005 UQ 513
Properties of the orbit ( animation )
Epoch:  April 27, 2019 ( JD 2,458,600.5)
Orbit type DO / E SDO or
CKBO («hot») ,
«Distant Object»
Major semi-axis 43.218  AU
eccentricity 0.147
Perihelion - aphelion 36.853 AU - 49.583 AU
Inclination of the orbit plane 25.7 °
Length of the ascending node 307.6 °
Argument of the periapsis 223 °
Time of passage of the perihelion June 7, 2124
Sidereal period 284 a 1.6 M.
Mean orbital velocity 4.494 km / s
Physical Properties
Medium diameter ${\ displaystyle 498 _ {- 75} ^ {+ 63} \ mathrm {km}}$
Albedo ${\ displaystyle 0 {,} 202 _ {- 0.049} ^ {+ 0.084} \ mathrm {}}$
Rotation period 7.03 h (0.293 d ) or
10.01 h (0.417 d)
Absolute brightness 3.50 - 3.87 mag
Spectral class C.
history
Explorer Michael E. Brown ,
David L. Rabinowitz
Date of discovery October 21, 2005
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.

(202421) 2005 UQ 513 is a large trans-Neptunian object in the Kuiper belt , which is classified dynamically as a Cubewano or as an extended Scattered Disc Object . Because of its size, the asteroid is a dwarf planet candidate .

## discovery

(202421) 2005 UQ 513 was discovered on October 21, 2005 by a team of astronomers consisting of Mike Brown ( CalTech ), Chad Trujillo ( Gemini ) and Dave Rabinowitz ( Yale ), as part of the Digitized Sky Survey project with the 1,2- m – Schmidt – Telescope discovered at the Palomar Observatory of the California Institute of Technology ( California ). The discovery was announced on September 1, 2007 together with 2003 UY 413 , 2003 UZ 413 , 2004 NT 33 , 2005 CA 79 and 2005 CB 79 , the planetoid was later given the minor planet number 202421 by the IAU .

After its discovery, UQ 513 could be identified on photos up to September 15, 1990, which were also taken at the Palomar Observatory as part of the Near Earth Asteroid Tracking Project (NEAT), and thus extended its observation period by 15 years so 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 October 2017, 206 observations were made over a period of 28 years from 17 oppositions. The last observation so far was made in November 2018 at the Purple Mountain Observatory . (As of February 22, 2019)

## properties

### Orbit

2005 UQ 513 orbits the sun in 284.13 years in an elliptical orbit between 36.85  AU and 49.58 AU from its center. The orbit eccentricity is 0.147, the orbit is inclined 25.70 ° with respect to the ecliptic . Currently, the planetoid is 48.02 AU from the sun. The next time it passes through perihelion in 2124, the last perihelion should have been in 1840.

Marc Buie ( DES ) classifies the planetoid as an extended SDO (ESDO or DO ), while the Minor Planet Center (MPC) and the Johnston's Archive him as Cubewano classifies, which is on the ground dynamically "hot" classical KBO would belong. The MPC generally lists it as a “Distant Object” and as a non-SDO.

### Size and rotation

The diameter of 2005 UQ 513 was determined to be 498 +63 in 2013 using combined data from the Herschel and Spitzer space telescopes−75 km determined. It is therefore possible that 2005 UQ 513 is in hydrostatic equilibrium due to its size and could therefore be largely round. However , it is not certain whether it meets the criteria for classification as a dwarf planet . Mike Brown believes that 2005 UQ 513 is most likely a dwarf planet. Gonzalo Tancredi did not give a recommendation in 2010 despite a diameter of 878 km he calculated.

The apparent magnitude of 2005 UQ 513 is 20.52  m .

Based on its light curve, the asteroid will most likely rotate once around its axis in 7.03 or 10.01 hours. The shorter rotation period is slightly more likely.

Determination of the diameter for 2005 UQ 513
year Dimensions km source
2010 878.0 Tancredi
2012 838.54 LightCurve DataBase
2014 498.0 +63.0-75.0 Vilenius et al. a.
2018 643.0 Brown
The most precise determination is marked in bold .

### surface

2005 UQ 513 shows a striking red color, which suggests the presence of significant amounts of tholines . It is therefore not a member of the Haumea collision family , although the orbit parameters would match.

## Individual evidence

1. ^ A b Marc W. Buie : Orbit Fit and Astrometric record for 202421 . SwRI (Space Science Department). Retrieved February 5, 2019.
2. a b MPC : MPEC 2010-S44: Distant Minor Planets (2010 OCT.11.0 TT) . IAU . September 25, 2010. Retrieved February 22, 2019.
3. a b c (202421) 2005 UQ513 at the IAU Minor Planet Center (English) Retrieved on February 22, 2019.
4. v ≈ π * a / period (1 + sqrt (1-e²))
5. E. Vilenius u. a .: “TNOs are cool”: A survey of the trans-Neptunian region X. Analysis of classical Kuiper belt objects from Herschel and Spitzer observations . In: Astronomy and Astrophysics . 541, No. A94, March 25, 2014, p. 17. arxiv : 1403.6309 . bibcode : 2014A & A ... 564A..35V . doi : 10.1051 / 0004-6361 / 201322416 .
6. a b A. Thirouin et al. a .: Short-term variability of 10 trans-Neptunian objects . In: Monthly Notices of the Royal Astronomical Society . 424, No. 4, August 21, 2012, pp. 3156-3177. arxiv : 1207.2044 . bibcode : 2012MNRAS.424.3156T . doi : 10.1111 / j.1365-2966.2012.21477.x .
7. a b LCDB Data for 2005 UQ513 . MinorPlanetInfo. August 2012. Retrieved February 22, 2019.
8. MPC : MPEC 2007-R02: 2003 UY413, 2003 UZ413, 2004 NT33, 2005 CA79, 2005 CB79, 2005 UQ513 . IAU . September 1, 2007. Retrieved February 22, 2019.
9. MPC : MPC / MPO / MPS Archive . IAU . Retrieved March 7, 2019.
10. (202421) 2005 UQ513 in the Small-Body Database of the Jet Propulsion Laboratory (English). Retrieved February 22, 2019.
11. ^ Wm. R. Johnston: List of Known Trans-Neptunian Objects . Johnston's Archives. October 7, 2018. Retrieved February 22, 2019.
12. MPC : MPEC List Of Centaurs and Scattered-Disk Objects . IAU . Retrieved February 22, 2019.
13. a b Mike Brown : How many dwarf planets are there in the outer solar system? . CalTech . November 12, 2018. Retrieved February 22, 2019.
14. a b Gonzalo 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 February 22, 2019.
15. AstDyS-2: (202421) 2005UQ513 . Universita di Pisa. Retrieved February 22, 2019.
16. Chad Trujillo et al. a .: A Photometric System for Detection of Water and Methane Ices on Kuiper Belt Objects . In: The Astrophysical Journal . 730, No. 2, March 10, 2011, p. 105. arxiv : 1102.1971 . ISSN 0004-637X . bibcode : 2011ApJ ... 730..105T . doi : 10.1088 / 0004-637X / 730/2/105 .
17. C. Snodgrass et al. a .: Characterization of candidate members of (136108) Haumea's family . In: EDP Sciences (Ed.): Astronomy and Astrophysics . 511, December 16, 2009, p. A72. arxiv : 0912.3171 . bibcode : 2010A & A ... 511A..72S . doi : 10.1051 / 0004-6361 / 200913031 .