2014 LO 28

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Asteroid
2014 LO 28
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 43,083  AU
eccentricity 0.118
Perihelion - aphelion 37.986 AU - 48.18 AU
Inclination of the orbit plane 25.5 °
Length of the ascending node 287.1 °
Argument of the periapsis 105.5 °
Time of passage of the perihelion January 28, 2058
Sidereal period 282 a 9.5 M.
Mean orbital velocity 4.501 km / s
Physical Properties
Medium diameter approx. 373 km
Albedo 0.08-0.09
Absolute brightness 5.4 - 5.6 mag
history
Explorer Pan-STARRS :
B. Gibson
T. Goggia
N. Primak
A. Schultz
M. Willman
Date of discovery June 1, 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 LO 28 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 railway dynamics. Due to its size, the asteroid may be one of the dwarf planet candidates .

discovery

2014 LO 28 was discovered on June 1, 2014 by an astronomical team 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 16, 2016.

After its discovery, in 2014 LO 28 could be identified on photos up to August 6, 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 September 2018, a total of 132 observations were made over a period of 9 years. The last observation so far was carried out again on the Pan-STARRS telescope (PS1) in August 2018. (As of March 14, 2019)

properties

Orbit

2014 LO 28 orbits the sun in 282.79 years on a slightly elliptical orbit between 37.99  AU and 48.18 AU from its center. The orbital eccentricity is 0.118, the web is 25.54 ° to the ecliptic inclined . The planetoid is currently 40.17 AU from the sun. He will next pass perihelion in 2058, so the last perihelion should have occurred in 1775.

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 373 km is currently assumed, based on a reflectivity of 8% and an absolute brightness of 5.6  m . Based on this diameter, the total surface area is around 437,000 km 2 . The apparent magnitude of 2014 LO 28 is 21.63  m .

Since it is conceivable that in 2014 LO 28 will be in hydrostatic equilibrium due to its size and thus could be largely round, it may meet the criteria for classification as a dwarf planet . Mike Brown believes that it is in 2014 LO 28 to perhaps is a dwarf planet.

Provisions of the diameter for 2014 LO 28
year Dimensions km source
2018 368.0 Johnston
2018 373.0 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 14LO28 . SwRI (Space Science Department). Retrieved March 14, 2019.
  2. ↑ a b c Wm. R. Johnston: List of Known Trans-Neptunian Objects . Johnston's Archives. October 7, 2018. Retrieved March 14, 2019.
  3. ↑ a b c 2014 LO28 at the IAU Minor Planet Center (English) Retrieved on March 14, 2019.
  4. ↑ v ≈ π * a / period (1 + sqrt (1-e²))
  5. ↑ MPC : MPEC 2016-048: 2014 LO28 . IAU . July 16, 2016. Accessed March 14, 2019.
  6. ↑ 2014 LO28 in the Small-Body Database of the Jet Propulsion Laboratory (English). Retrieved March 14, 2019. Template: JPL Small-Body Database Browser / Maintenance / Alt
  7. ↑ MPC : MPEC List Of Centaurs and Scattered-Disk Objects . IAU . Retrieved March 14, 2019.
  8. ↑ 2014 LO28 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 14, 2019.