2014 BZ 57

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Asteroid
2014 BZ 57
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 42.786  AU
eccentricity 0.14
Perihelion - aphelion 36.792 AU - 48.78 AU
Inclination of the orbit plane 27.1 °
Length of the ascending node 274.6 °
Argument of the periapsis 265.3 °
Time of passage of the perihelion June 15, 2036
Sidereal period 279 a 10.4 M
Mean orbital velocity 4.516 km / s
Physical Properties
Medium diameter approx. 479 km
Albedo 0.07-0.09
Absolute brightness 5.0 - 5.2 mag
history
Explorer La Silla Observatory
Date of discovery January 24, 2014
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.

2014 BZ 57 is a large trans-Neptunian object in the Kuiper Belt , which is classified as an extended Scattered Disk Object or as a Cubewano in terms of orbital dynamics . Because of its size, the asteroid is a dwarf planet candidate .

discovery

2014 BZ 57 was discovered on January 24, 2014 by a team of astronomers using the 3.6 m telescope of the European Southern Observatory at the La Silla Observatory ( Chile ). The discovery was announced on July 15, 2016.

After its discovery, in 2014 BZ 57 could be identified on photos taken as part of the Near Earth Asteroid Tracking Program at the Palomar Observatory up to December 11, 2002, thus extending its observation period by 12 years calculate its orbit more precisely. In September 2018, a total of 213 observations over a period of 16 years were available. The last observation so far was carried out in March 2018 as part of the Pan-STARRS project. (As of February 24, 2019)

properties

Orbit

2014 BZ 57 orbits the sun in 279.87 years on a slightly elliptical orbit between 36.79  AU and 48.78 AU from its center. The orbital eccentricity is 0.140, the orbit is 27.05 ° inclined to the ecliptic . The planetoid is currently 42.38 AU from the sun. He will next pass perihelion in 2036, so the last perihelion should have occurred in 1756.

Marc Buie ( DES ) classifies the planetoid as an extended SDO (ESDO or DO ), while the Minor Planet Center 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 and rotation

A diameter of around 479 km is currently assumed, based on a reflectivity of 7% and an absolute brightness of 5.2  m . The apparent magnitude of 2014 BZ 57 is 20.81  m .

Since it can be assumed that 2014 BZ 57 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 it is in 2014 BZ 57 to possibly is a dwarf planet.

Provisions of the diameter for 2014 BZ 57
year Dimensions km source
2018 443.0 Johnston
2018 479.0 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 14BZ57 . SwRI (Space Science Department). Retrieved February 25, 2019.
  2. ↑ a b c Wm. R. Johnston: List of Known Trans-Neptunian Objects . Johnston's Archives. October 7, 2018. Retrieved February 25, 2019.
  3. ↑ a b c 2014 BZ57 at the IAU Minor Planet Center (English) Retrieved on February 25, 2019.
  4. ↑ v ≈ π * a / period (1 + sqrt (1-e²))
  5. ↑ MPC : MPEC 2016-N126: 2014 BZ57 . IAU . July 15, 2016. Retrieved February 25, 2019.
  6. ↑ 2014 BZ57 in the Small-Body Database of the Jet Propulsion Laboratory (English). Retrieved February 25, 2019. Template: JPL Small-Body Database Browser / Maintenance / Alt
  7. ↑ MPC : MPEC List Of Centaurs and Scattered-Disk Objects . IAU . Retrieved February 25, 2019.
  8. ↑ 2014 BZ57 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 February 25, 2019.