(455502) 2003 UZ 413

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Asteroid
(455502) 2003 UZ 413
Properties of the orbit ( animation )
Epoch:  April 27, 2019 ( JD 2,458,600.5)
Orbit type Plutino ,
"Distant Object"
Major semi-axis 39.104  AU
eccentricity 0.227
Perihelion - aphelion 30.241 AU - 47.968 AU
Inclination of the orbit plane 12 °
Length of the ascending node 135.9 °
Argument of the periapsis 145 °
Time of passage of the perihelion April 7, 1942
Sidereal period 224 a 6.5 M
Mean orbital velocity 4.724 km / s
Physical Properties
Medium diameter approx. 536 km
Albedo 0.08-0.09
Medium density 2.645 ± 0.355 g / cc
Rotation period 4.13 ± 0.05 h (0.1721 d )
Absolute brightness 4.36 ± 0.06 mag
Spectral class C
V-R = 0.450 ± 0.057
history
Explorer Michael E. Brown,
David L. Rabinowitz,
Chadwick A. Trujillo
Date of discovery October 21, 2003
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.

(455502) 2003 UZ 413 is a large trans-Neptunian object that is classified as Plutino (2: 3 - resonant KBO ) in terms of orbital dynamics . Due to its size, the asteroid is one of the dwarf planet candidates . With a rotation time of just over 4 hours, it is the second fastest rotating celestial body in the solar system after Haumea .

discovery

(455502) 2003 UZ 413 was discovered on October 21, 2003 by a team of astronomers consisting of Mike Brown ( CalTech ), Chad Trujillo ( Gemini Observatory ) and Dave Rabinowitz ( Yale University ), as part of near-earth asteroid tracking Project (NEAT) discovered with the 1.2 m Oschin Schmidt telescope at the Palomar Observatory ( California ). The discovery was announced on September 1, 2007 along with 2003 UY 413 , 2004 NT 33 , 2005 CA 79 , 2005 CB 79, and 2005 UQ 513 . He received from the IAU , the Minor Planet -number 455502 .

After its discovery, UZ 413 could be identified back in 2003 on photos from July 29, 1954, which were also taken at the Palomar Observatory as part of the Digitized Sky Survey program (DSS) , and its observation period was extended by 49 years and so his Calculate orbit more accurately. Since then, UZ 413 has been observed with earth-based telescopes in 2003 . In November 2017, there were a total of 160 observations over a period of 64 years. The last observation so far was carried out in October 2017 on the 1.8 m Pan-STARRS telescope (PS1). (As of March 7, 2019)

properties

Simulation of the orbit from 2003 UZ 413 .

Orbit

2003 UZ 413 orbits the sun in 244.54 years in an elliptical orbit between 30.24  AU and 47.97 AU from its center. The orbital eccentricity is 0.227, the orbit is 12.05 ° inclined to the ecliptic . The planetoid is currently 44.06 AU from the Sun. The asteroid passed perihelion for the last time in 1942; the next perihelion should therefore take place around the year 2186.

Both Marc Buie ( DES ) and the Minor Planet Center classify the planetoid as Plutino ; the latter also lists it as a non-SDO and generally as a “distant object”.

Size and rotation

A calculated diameter of 536 km is currently assumed; this value is based on an assumed reflectivity of 8% and an absolute brightness of 4.7  m . It can therefore be assumed that 2003 UZ 413 is in hydrostatic equilibrium and the asteroid is therefore a dwarf planet candidate , based on Mike Brown's taxonomic 5-class system , from which this assessment comes. Mike Brown assumes that 2003 UZ 413 is likely a dwarf planet. Assuming a diameter of 536 km, this results in a total surface of around 903,000 km 2 .

2003 UZ 413 rotates once around its axis in 4 hours and 7.8 minutes. It follows that in a 2003 UZ 413 year, he performs 519,035.1 self- rotations ("days"). The JPL states 4.14 hours. Due to the rapid rotation, the mean density must exceed 0.72 g / cm 3 , otherwise the structure of the asteroid would not be stable. Stable Jacobi ellipsoids with an axis rate of ≥ 1.13 ± 0.03, as implied by its light curve amplitude of Δm = 0.13 ± 0.03, exist for average densities of 2.29-3.00 g / cm 3 . Accordingly, 2003 UZ 413 , similar to Haumea, Varuna or 2008 OG 19 , should have an elongated shape at the equator.

In visible light, 2003 UZ 413 has a neutral or slightly reddish color with a flat, structureless spectrum. The apparent magnitude of 2003 UZ 413 is 20.99  m .

Determinations of the diameter for 2003 UZ 413
year Dimensions km source
2010 580.0 Tancredi
2010 580.13 LightCurve DataBase
2018 612.0 Johnston
2018 536.0 Brown
The most precise determination is marked in bold .

See also

Web links

Individual evidence

  1. ^ A b Marc W. Buie : Orbit Fit and Astrometric record for 455502 . SwRI (Space Science Department). Retrieved March 7, 2019.
  2. ↑ a b MPC : MPEC 2010-S44: Distant Minor Planets (2010 OCT.11.0 TT) . IAU . September 25, 2010. Retrieved March 7, 2019.
  3. ↑ a b c Wm. R. Johnston: List of Known Trans-Neptunian Objects . Johnston's Archives. October 7, 2018. Retrieved March 7, 2019.
  4. ↑ a b c (455502) 2003 UZ413 at the IAU Minor Planet Center (English) Retrieved March 7, 2019.
  5. ↑ v ≈ π * a / period (1 + sqrt (1-e²))
  6. ↑ a b D. Perna et al. a .: Rotations and densities of trans-Neptunian objects (PDF) . In: Astronomy and Astrophysics . 508, No. 1, July 12, 2009, pp. 451-455. bibcode : 2009A & A ... 508..451P . doi : 10.1051 / 0004-6361 / 200911970 .
  7. ↑ D. Perna et al. a .: Light Curves and Densities of Centaurs and Trans-Neptunian Objects from the ESO Large Program . In: American Astronomical Society, DPS meeting . 40, September 2008, p. 483. bibcode : 2008DPS .... 40.4708P .
  8. ↑ a b D. Perna et al. a .: Colors and taxonomy of Centaurs and trans-Neptunian objects (PDF) . In: Astronomy and Astrophysics . 510, No. A53, February 2010. arxiv : 0912.2621 . bibcode : 2010A & A ... 510A..53P . doi : 10.1051 / 0004-6361 / 200913654 .
  9. ↑ a b LCDB Data for (455502) 2003UZ413 . MinorPlanetInfo. 2012. Retrieved March 7, 2019.
  10. ↑ MPC : MPEC 2007-R02: 2003 UY413, 2003 UZ413, 2004 NT33, 2005 CA79, 2005 CB79, 2005 UQ513 . IAU . September 1, 2007. Accessed March 7, 2019.
  11. ↑ MPC : MPC / MPO / MPS Archive . IAU . Retrieved March 7, 2019.
  12. ↑ (455502) 2003 UZ413 in the Small-Body Database of the Jet Propulsion Laboratory (English). Retrieved March 7, 2019. Template: JPL Small-Body Database Browser / Maintenance / Alt
  13. ↑ MPC : MPEC List Of Centaurs and Scattered-Disk Objects . IAU . Retrieved March 7, 2019.
  14. ↑ a b Mike Brown : How many dwarf planets are there in the outer solar system? . CalTech . November 12, 2018. Retrieved March 7, 2019.
  15. ↑ (455502) 2003 UZ413 in the database of the "Asteroids - Dynamic Site" (AstDyS-2, English).
  16. ^ 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 7, 2019.