(523736) 2014 QA 442

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Asteroid
(523736) 2014 QA 442
Properties of the orbit ( animation )
Epoch:  April 27, 2019 ( JD 2,458,600.5)
Orbit type SDO or
DO (E SDO ) or
CKBO ( «Hot» ),
«Distant Object»
Major semi-axis 43.101  AU
eccentricity 0.182
Perihelion - aphelion 35.277 AU - 50.925 AU
Inclination of the orbit plane 27.4 °
Length of the ascending node 109.3 °
Argument of the periapsis 281.3 °
Time of passage of the perihelion November 21, 2029
Sidereal period 282 a 11.6 M
Mean orbital velocity 4,500 km / s
Physical Properties
Medium diameter approx. 358 km
Albedo 0.08-0.09
Absolute brightness 5.5 - 5.7 mag
history
Explorer Pan-STARRS
Date of discovery September 8, 2010
Another name 2010 TR 19
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.

(523736) 2014 QA 442 is a large trans-Neptunian object in the Kuiper belt , which is classified as a near or extended scattered disk object (SDO or DO) or as a Cubewano (CKBO) in terms of orbital dynamics. Due to its size, the asteroid may be one of the dwarf planet candidates .

discovery

2014 QA 442 was first discovered on September 8, 2010 by a team of astronomers as part of the Pan-STARRS project at the Haleakalā Observatory ( Maui ), it was given the provisional designation 2010 TR 19 . For some time in 2010, TR 19 was considered a lost centaur , believed to have a perihelion of around 11 AU. Because of its great absolute magnitude of 5.3 mag, there was a possibility that it is even larger than the lost centaur 1995 SN 55 . Then on August 16, 2014 the planetoid 2014 QA 442 was discovered. In June 2017 it was surprisingly declared that 2010 TR 19 and 2014 QA 442 are the same planetoid, but not a centaur, but an ordinary trans-Neptunian Kuiper belt planetoid. He received on 25 September 2018 the IAU , the Minor Planet -number five hundred and twenty-three thousand seven hundred thirty-six .

The observation arc of the planetoid begins with the official observation on September 8, 2010. Since then, the planetoid has been observed through various earth-based telescopes. In October 2018, a total of 92 observations were made over a period of 8 years. The last observation so far was made in November 2018 at the Purple Mountain Observatory ( China ). (As of March 18, 2019)

properties

Orbit

2014 QA 442 orbits the sun in 282.97 years on a slightly elliptical orbit between 35.27  AU and 50.93 AU from its center. The orbital eccentricity is 0.182, the orbit is 27.40 ° inclined to the ecliptic . The planetoid is currently 35.60 AU from the sun. He will next pass perihelion in 2029, so the last perihelion should have occurred in 1746.

Marc Buie ( DES ) classifies the asteroid as a near ( SDO ) or extended SDO (ESDO or DO ), while the Minor Planet Center does not have a specific classification; the latter classifies it as a non-SDO and generally as a “distant object” . The Johnston's Archive, however, lists him as Cubewano , whereby he would belong to the "hot" classic KBO in terms of rail dynamics .

size

A diameter of 358 km is currently assumed, based on a reflectivity of 8% and an absolute brightness of 5.7  m . Based on this diameter, the total surface area is around 403,000 km 2 . The apparent magnitude of 2014 QA 442 is 21.19  m .

Since it is conceivable that 2014 QA 442 is in hydrostatic equilibrium due to its size and could thus be largely round, it may meet the criteria for classification as a dwarf planet . Mike Brown believes that it is in 2014 QA 442 to perhaps is a dwarf planet.

Provisions of the diameter for 2014 QA 442
year Dimensions km source
2018 352.0 Johnston
2018 358.0 Brown
The most precise determination is marked in bold .

See also

Web links

Individual evidence

  1. ↑ a b c Marc W. Buie : Orbit Fit and Astrometric record for 523736 . SwRI (Space Science Department). Retrieved March 18, 2019.
  2. ↑ a b c Wm. R. Johnston: List of Known Trans-Neptunian Objects . Johnston's Archives. October 7, 2018. Retrieved March 18, 2019.
  3. ↑ a b c (523736) 2014 QA442 at the IAU Minor Planet Center (English) Retrieved March 18, 2019.
  4. ↑ v ≈ π * a / period (1 + sqrt (1-e²))
  5. ↑ J. Parker: Distant EKOs, The Kuiper Belt Electronic Newsletter . No. 109 , June 2017 (English, boulder.swri.edu [PDF; 91 kB ]).
  6. ↑ MPC : MPC / MPO / MPS Archive . IAU . Retrieved March 18, 2019.
  7. ↑ (523736) 2014 QA442 in the Small-Body Database of the Jet Propulsion Laboratory (English). Retrieved March 18, 2019. Template: JPL Small-Body Database Browser / Maintenance / Alt
  8. ↑ MPC : MPEC List Of Centaurs and Scattered-Disk Objects . IAU . Retrieved March 18, 2019.
  9. ↑ (523736) 2014 QA442 in the database of the "Asteroids - Dynamic Site" (AstDyS-2, English).
  10. ↑ a b Mike Brown : How many dwarf planets are there in the outer solar system? . CalTech . November 12, 2018. Retrieved March 18, 2019.