2014 BX ₆₄

Asteroid 2014 BX 64
Properties of the orbit ( animation ) Epoch:  April 27, 2019 ( JD 2,458,600.5)
Orbit type	CKBO  ( "Hot" ) "Distant Object"
Major semi-axis	41.753  AU
eccentricity	0.046
Perihelion - aphelion	39.846 AU - 43.661 AU
Inclination of the orbit plane	11.2 °
Length of the ascending node	323.1 °
Argument of the periapsis	74.9 °
Time of passage of the perihelion	September 26, 1946
Sidereal period	269 a 9.6 M
Mean orbital velocity	4.572 km / s
Physical Properties
Medium diameter	approx. 315 km
Albedo	0.08-0.09
Absolute brightness	5.8 - 5.9 mag
history
Explorer	Pan-STARRS : B. Gibson T. Goggia N. Primak A. Schultz M. Willman
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 BX ₆₄ is a large trans-Neptunian object in the Kuiper Belt , which is classified as Cubewano (CKBO) in terms of railway dynamics . Due to its size, the asteroid is one of the dwarf planet candidates .

discovery

2014 BX ₆₄ was tested on January 24, 2014 by a team of astronomers consisting of B. Gibson, T. Goggia, N. Primak, A. Schultz and M. Willman, as part of the Pan-STARRS project with the 1.8 m -Ritchey Chretien Telescope (PS1) discovered at Haleakalā Observatory ( Maui ). The discovery was announced on July 17, 2016.

After its discovery, in 2014 BX _{64 could be identified} on photos taken as part of the Sloan Digital Sky Survey program (SDSS) at the Apache Point Observatory ( New Mexico ) going back to January 14, 2002, thus changing its observation period Extend twelve years to more accurately calculate its orbit. So far, the planetoid has only been observed by the Pan-STARRS and the Apache Point observatory. In September 2018, there were a total of 161 observations over a period of 17 years. The last observation so far was carried out again at the Pan-STARRS telescope in March 2018. (As of March 27, 2019)

properties

Orbit

2014 BX ₆₄ orbits the sun in 269.80 years in an almost circular orbit between 39.84  AU and 43.66 AU from its center. The orbital eccentricity is 0.046, the orbit is 11.17 ° inclined to the ecliptic . The planetoid is currently 42.06 AU from the Sun. He passed through perihelion for the last time in 1946, so the next perihelion should take place in 2216.

Marc Buie ( DES ) classifies the asteroid as Cubewano , whereby it belongs to the orbital dynamics “hot” classical KBO , while the Minor Planet Center does not have a specific classification; it classifies it as a non-SDO and generally as a “distant object” .

size

A diameter of 315 km is currently assumed, based on a reflectivity of 8% and an absolute brightness of 5.9  ^m . Based on this diameter, the total surface area is around 312,000 km ² . The apparent magnitude of 2014 BX ₆₄ is 22.21  ^m .

Since it is conceivable that 2014 BX ₆₄ 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 believes that it is in 2014 BX ₆₄ to perhaps is a dwarf planet.

Provisions of the diameter for 2014 BX ₆₄

year	Dimensions km	source
2018	306.0	Johnston
2018	315.0	Brown
The most precise determination is marked in bold .

See also

• List of trans-Neptunian objects
• List of dwarf planets of the solar system
• List of asteroids
• List of moons from asteroids

Web links

• How many dwarf planets are there in the outer solar system? Current list of the largest TNOs from Mike Brown
• Free the dwarf planets! Mike Brown's column on the IAU and the dwarf planets regarding their classifications (23 August 2011)

Individual evidence

1. ^ ^{A b} Marc W. Buie : Orbit Fit and Astrometric record for 14BX64 . SwRI (Space Science Department). Retrieved March 27, 2019.
2. ↑ ^{a b c} Wm. R. Johnston: List of Known Trans-Neptunian Objects . Johnston's Archives. October 7, 2018. Retrieved March 27, 2019.
3. ↑ ^{a b c} 2014 BX64 at the IAU Minor Planet Center (English) Accessed March 27, 2019.
4. ↑ v ≈ π * a / period (1 + sqrt (1-e²))
5. ↑ MPC : MPEC 2016-O124: 2014 BX64 . IAU . July 17, 2016. Accessed March 27, 2019.
6. ↑ 2014 BX64 in the Small-Body Database of the Jet Propulsion Laboratory (English). Retrieved March 27, 2019.
7. ↑ MPC : MPEC List Of Centaurs and Scattered-Disk Objects . IAU . Retrieved March 27, 2019.
8. ↑ 2014 BX64 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 27, 2019.