2010 JO 179

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Asteroid
2010 JO 179
Properties of the orbit ( animation )
Epoch:  April 27, 2019 ( JD 2,458,600.5)
Orbit type SDO or RKBO 5:21
Major semi-axis 79.141  AU
eccentricity 0.5
Perihelion - aphelion 39.608 AU - 118.674 AU
Inclination of the orbit plane 32 °
Length of the ascending node 147.3 °
Argument of the periapsis 10.7 °
Time of passage of the perihelion March 9, 1952
Sidereal period 704 a 0.7 M.
Physical Properties
Medium diameter approx. 600 km
Albedo 0.09-0.10
Rotation period 30.6 h
Absolute brightness 3.4 - 4.3 mag
history
Explorer Pan-STARRS
Date of discovery May 10, 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 JO 179 is a trans-Neptunian object that is classified as SDO or as a resonant KBO ( 5:21 resonance). The celestial body is currently one of the largest objects that has not yet received a minor planet number from the IAU . Because of its size, the asteroid is a dwarf planet candidate .

discovery

2010 JO 179 was discovered as part of the Pan-STARRS -Outer Solar System Survey program at the Haleakala Observatory on Maui ( Hawaii ). Its discovery was announced on September 15, 2017 by a team of astronomers led by Matthew J. Holman and three days later by the Minor Planet Center .

After its discovery on photos taken on May 10, 2010, JO 179 could be identified in photos from May 11, 2005 and thus its orbit calculated more precisely. Since then, JO 179 has been observed with earth-based telescopes in 2010 . In December 2018, there were a total of 125 observations over a period of 13 years.

properties

2010 orbit JO 179 (white) compared to other distant asteroids.

Orbit

2010 JO 179 orbits the sun in 704.06 years on a strongly elliptical orbit between 39.61  AU and 118.67 AU from its center. The orbital eccentricity is 0.500, the orbit is 32.03 ° inclined to the ecliptic . The asteroid is currently close to its aphelion, about 80 AU away. The last run of the perihelion took place in 1952; the next would have to happen in the year 2656.

The MPC classifies 2010 JO 179 as a Scattered Disc Object , while the discoverers classify it as RKBO with a 5:21 response.

size

It is currently assumed to have a diameter of around 600 km; it can therefore be assumed that 2010 JO 179 is in hydrostatic equilibrium and that the asteroid thus belongs to the dwarf planet candidates , based on Mike Brown's taxonomic 5-class system . The latter himself estimates the diameter of the asteroid at 574 km based on an assumed albedo of 9% and an absolute brightness of 4.5  m . Since this estimate is less than 600 km, Brown assumes that 2010 JO 179 is only likely to be a dwarf planet. The explorers estimate the diameter of the asteroid at 600 to 900 km.

2010 JO 179 rotates exceptionally slowly around its axis in 1 day, 6 hours and 36 minutes. It follows that the planetoid performs 201,692.2 self- rotations (“days”) in a 2010 JO 179 year .

Monomodal light curve observations indicated, in addition to the rotation period of 30.6 hours, a rather round shape with significant albedo spots. An alternative rotating solution of a bimodal light curve is considered less likely. This would double the period of rotation and imply an ellipsoidal shape with an axis rate of at least 1.58.

Provisions of the diameter for 2010 JO 179
year Dimensions km source
2017 600-900 Holman  et al. a.
2018 702.0 Johnston
2018 574.0 Brown
The most precise determination is marked in bold .

See also

Individual evidence

  1. ↑ Andreas Müller: Astronomers discover other dwarf planets in the solar system (September 2017)
  2. ↑ MPC : MPEC 2017-S54: 2010 JO179 (September 2017)
  3. ↑ MPC : List Of Centaurs and Scattered-Disk Objects (January 2019)
  4. ↑ M. Holman : A dwarf planet class object in the 21: 5 resonance with Neptune (September 2017, PDF)
  5. ↑ Johnston's Archives: List of Known Trans-Neptunian Objects (October 2018)
  6. ↑ M. Brown : How many dwarf planets are there in the outer solar system? (November 2018)