(303775) 2005 QU 182

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Asteroid
(303775) 2005 QU 182
Properties of the orbit ( animation )
Epoch:  April 27, 2019 ( JD 2,458,600.5)
Orbit type SDO ,
"Distant Object"
Major semi-axis 112.535  AU
eccentricity 0.673
Perihelion - aphelion 36.793 AU - 188.276 AU
Inclination of the orbit plane 14 °
Length of the ascending node 78.3 °
Argument of the periapsis 224 °
Time of passage of the perihelion July 14, 1971
Sidereal period 1193 a 9.8 m
Mean orbital velocity 2.785 km / s
Physical Properties
Medium diameter
Albedo
Rotation period 9.61 ± 0.05 h (0.400 d )
Absolute brightness 3.80 ± 0.32 mag
Spectral class C
B-V = 0.940 ± 0.030
VR = 0.540 ± 0.030
VI = 1.050 ± 0.042
history
Explorer Michael E. Brown ,
Chadwick A. Trujillo,
David L. Rabinowitz
Date of discovery August 30, 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.

(303775) 2005 QU 182 is a large trans-Neptunian object that is classified as a Scattered Disk Object (SDO) in terms of orbital dynamics . Because of its size, the asteroid is a dwarf planet candidate .

discovery

2005 QU 182 was developed on August 30, 2005 by a team of astronomers consisting of Mike Brown ( CalTech ), Chad Trujillo ( Gemini Observatory ) and Dave Rabinowitz ( Yale University ), as part of the Near Earth Asteroid Tracking Project ( NEAT) discovered at the 1.2 m Oschin Schmidt telescope of the Palomar Observatory ( California ). The discovery was announced on September 1, 2007 together with 2004 PF 115 , 2004 PG 115 and 2004 XA 192 , the planetoid was later given the minor planet number 303775 by the IAU .

After its discovery, QU 182 could be identified in photos up to June 17, 1974, taken as part of the Digitized Sky Survey program (DSS) at the Siding Spring Observatory , and thus its observation period was extended by 22 years in order to calculate its orbit more precisely. In April 2017, there were a total of 158 observations over a period of 41 years. The last observation so far was carried out in September 2017 on the Pan-STARRS telescope (PS1). (As of March 7, 2019)

properties

The orbit of 2005 QU 182 (blue, light blue) compared to Pluto and the giant planets (white, gray).

Orbit

2005 QU 182 orbits the sun in 1193.82 years on a strongly elliptical orbit between 36.79  AU and 188.28 AU from its center. The orbit eccentricity is 0.673, the orbit is inclined 14.05 ° with respect to the ecliptic . The planetoid is currently 53.04 AU from the Sun. He passed through perihelion for the last time in 1971, so the next perihelion should take place in 3165.

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

Size and rotation

A diameter of 416 km is currently assumed, based on a reflectivity of 32.8% and an absolute brightness of 3.8  m . Assuming a diameter of 416 km, this results in a total surface of around 544,000 km². The apparent magnitude of 2005 QU 182 is 21.14  m .

Since it can be assumed that 2005 QU 182 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 2005 QU 182 may be a dwarf planet. Gonzalo Tancredi did not make a recommendation in 2010, despite a diameter of over 1000 km that he calculated at the time.

Using light curve observations , the 2005 QU 182 rotates once around its axis in 9 hours and 36.6 minutes. It follows that in a 2005 QU 182 year it performs 1,088,972.1 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%.

Determinations of the diameter for 2005 QU 182
year Dimensions km source
2010 1008.0 Tancredi
2012 800.80 LightCurve DataBase
2012 416.0 ± 73.0 Santos-Sanz et al. a.
2018 415.0 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 303775 . SwRI (Space Science Department). Retrieved March 7, 2019.
  2. ↑ a b MPC : MPEC List Of Centaurs and Scattered-Disk Objects . IAU . Retrieved March 7, 2019.
  3. ^ A b Wm. R. Johnston: List of Known Trans-Neptunian Objects . Johnston's Archives. October 7, 2018. Retrieved March 7, 2019.
  4. ↑ a b c (303775) 2005 QU182 at the IAU Minor Planet Center (English) Accessed March 7, 2019.
  5. ↑ v ≈ π * a / period (1 + sqrt (1-e²))
  6. ↑ a b c d P. Santos-Sanz u. a .: “TNOs are Cool”: A survey of the trans-Neptunian region. IV. Size / albedo characterization of 15 scattered disk and detached objects observed with Herschel-PACS (PDF) . In: Astronomy and Astrophysics . 541, No. A92, May 4, 2012, p. 18. arxiv : 1202.1481 . bibcode : 2012A & A ... 541A..92S . doi : 10.1051 / 0004-6361 / 201118541 .
  7. ↑ S. Benecchi, S. Sheppard : Light Curves of 32 Large Transneptunian Objects (PDF) . In: The Astronomical Journal . 145, No. 5, January 24, 2013, p. 124, 19. arxiv : 1301.5791 . bibcode : 2013AJ .... 145..124B . doi : 10.1088 / 0004-6256 / 145/5/124 .
  8. ↑ a b LCDB Data for (303775) 2005QU182 . MinorPlanetInfo. 2014. Retrieved March 7, 2019.
  9. ↑ a b c 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 2007-R03: 2004 PF115, 2004 PG115, 2004 XA192, 2005 QU182 . IAU . September 1, 2007. Accessed March 7, 2019.
  11. ↑ MPC : MPC / MPO / MPS Archive . IAU . Retrieved March 7, 2019.
  12. ↑ (303775) 2005 QU182 in the Small-Body Database of the Jet Propulsion Laboratory (English). Retrieved March 7, 2019. Template: JPL Small-Body Database Browser / Maintenance / Alt
  13. ↑ (303775) 2005 QU182 in the database of the "Asteroids - Dynamic Site" (AstDyS-2, English).
  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. ^ 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 7, 2019.