(535228) 2014 YE 50

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Asteroid
2014 YE 50
Properties of the orbit ( animation )
Epoch:  April 27, 2019 ( JD 2,458,600.5)
Orbit type SDO ,
"Distant Object"
Major semi-axis 59.103  AU
eccentricity 0.376
Perihelion - aphelion 36,901 AU - 81,305 AU
Inclination of the orbit plane 26.9 °
Length of the ascending node 121.2 °
Argument of the periapsis 286.7 °
Time of passage of the perihelion August 29, 1966
Sidereal period 454 a 4.6 M
Mean orbital velocity 3.843 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 December 21, 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 YE 50 is a large trans-Neptunian object that is classified as a Scattered Disk Object (SDO) in terms of its orbit dynamics . Due to its size, the asteroid may be one of the dwarf planet candidates .

discovery

2014 YE 50 was discovered on December 21, 2014 by a team of astronomers as part of the Pan-STARRS project with the 1.8 m Ritchey Chretien telescope (PS1) at the Haleakalā Observatory ( Maui ). The discovery was announced on July 17, 2016 by a Pan-STARRS team of astronomers consisting of B. Gibson, T. Goggia, N. Primak, A. Schultz, and M. Willman.

After its discovery, in 2014 YE 50 could be identified in photos up to April 3, 2010, which were also taken as part of the Pan-STARRS program, and thus its observation period was extended by four years in order to calculate its orbit more precisely. So far, the planetoid has only been observed through the Pan-STARRS telescope. In December 2018, there were a total of 123 observations over a period of 8 years. The last observation so far was carried out again on the Pan-STARRS telescope (PS1) in February 2018. (As of March 18, 2019)

properties

Orbit

2014 YE 50 orbits the sun in 454.38 years on a strongly elliptical orbit between 36.90  AU and 81.30 AU from its center. The orbital eccentricity is 0.376, the orbit is inclined 26.92 ° to the ecliptic . Currently, the planetoid is 48.11 AU from the sun. He last passed through perihelion in 1966, so the next perihelion should take place in 2421.

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

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 YE 50 is 22.42  m .

Since it is conceivable that 2014 YE 50 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 2014 YE 50 to perhaps is a dwarf planet.

Provisions of the diameter for 2014 YE 50
year Dimensions km source
2018 386.0 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 14YE50 . SwRI (Space Science Department). Retrieved March 18, 2019.
  2. ↑ a b MPC : MPEC List Of Centaurs and Scattered-Disk Objects . IAU . Retrieved March 18, 2019.
  3. ↑ a b c Wm. R. Johnston: List of Known Trans-Neptunian Objects . Johnston's Archives. October 7, 2018. Retrieved March 18, 2019.
  4. ↑ a b c (535228) 2014 YE50 at the IAU Minor Planet Center (English) Retrieved March 18, 2019.
  5. ↑ v ≈ π * a / period (1 + sqrt (1-e²))
  6. ↑ MPC : MPEC 2016-O252: 2014 YE50 . IAU . July 17, 2016. Accessed March 18, 2019.
  7. ↑ (535228) 2014 YE50 in the Small-Body Database of the Jet Propulsion Laboratory (English). Retrieved March 18, 2019. Template: JPL Small-Body Database Browser / Maintenance / Alt
  8. ↑ (535228) 2014 YE50 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.