2010 VQ 11

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Asteroid
2010 VQ 11
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 44,927  AU
eccentricity 0.136
Perihelion - aphelion 38.805 AU - 51.05 AU
Inclination of the orbit plane 13.3 °
Length of the ascending node 174.8 °
Argument of the periapsis 213.2 °
Time of passage of the perihelion 1st December 1985
Sidereal period 301 a 1.8 M.
Mean orbital velocity 4.407 km / s
Physical Properties
Medium diameter approx. 358 km
Albedo 0.08-0.09
Absolute brightness 5.6 - 5.7 mag
history
Explorer David L. Rabinowitz , Megan E. Schwamb, Suzanne W. Tourtellotte
Date of discovery November 2, 2010
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.

2010 VQ 11 is a large trans-Neptunian object in the Kuiper Belt , which is classified as an extended Scattered Disk Object (DO) or as a Cubewano (CKBO) in terms of orbital dynamics. Due to its size, the asteroid is one of the dwarf planet candidates .

discovery

2010 VQ 11 was discovered on November 2, 2010 by a team of astronomers consisting of Dave Rabinowitz , Meg Schwamb and Suzanne Tourtellotte with the 3.6 m ESO telescope at the La Silla Observatory ( Chile ) of the European Southern Observatory (ESO) discovered. The discovery was announced on March 17, 2012 after confirmation by the 1.3 m reflector telescope at the Cerro Tololo Observatory (Chile).

After its discovery in 2010, VQ 11 could be identified on photos taken as part of the Near Earth Asteroid Tracking Program (NEAT) at the Palomar Observatory ( California ) going back to December 7, 2002, thus extending its observation period by eight years in order to calculate its orbit more precisely. Since then, the planetoid has been observed through various earth-based telescopes. In September 2018, a total of 151 observations were made over a period of 15 years. The last observation so far was carried out in February 2017 on the Pan-STARRS telescope (PS1). (As of March 18, 2019)

properties

Orbit

2010 VQ 11 orbits the sun in 301.15 years on a slightly elliptical orbit between 38.80  AU and 51.05 AU from its center. The orbit eccentricity is 0.136, the orbit is inclined 13.31 ° to the ecliptic . The planetoid is currently 40.62 AU from the sun. He last passed through perihelion in 1985, so the next perihelion should take place in 2287.

Marc Buie ( DES ) classifies the planetoid as an 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 area is about 403,000 km². The apparent magnitude of 2010 VQ 11 is 21.92  m .

Since it is conceivable that 2010 VQ 11 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 expects that it is at 2010 VQ 11 to perhaps is a dwarf planet.

Determination of the diameter for 2010 VQ 11
year Dimensions km source
2018 336.0 Johnston
2018 358.0 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 10VQ11 . 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 2010 VQ11 at the IAU Minor Planet Center (English) Retrieved March 18, 2019.
  4. ↑ v ≈ π * a / period (1 + sqrt (1-e²))
  5. ↑ MPC : MPEC 2012-F15: 2010 VQ11 . IAU . March 17, 2012. Retrieved March 18, 2019.
  6. ↑ 2010 VQ11 in the Small-Body Database of the Jet Propulsion Laboratory (English). Retrieved March 18, 2019. Template: JPL Small-Body Database Browser / Maintenance / Alt
  7. ↑ MPC : MPEC List Of Centaurs and Scattered-Disk Objects . IAU . Retrieved March 18, 2019.
  8. ↑ 2010 VQ11 in the database of the "Asteroids - Dynamic Site" (AstDyS-2, English).
  9. ↑ a b Mike Brown : How many dwarf planets are there in the outer solar system? . CalTech . November 12, 2018. Retrieved March 18, 2019.