(668643) 2012 DR30

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(668643) 2012 DR30
2012 DR30 SDSS precovery.png
2012 DR30 in a precovery image taken by the Sloan Digital Sky Survey in 2000
Discovery [1]
Discovered by PMO NEO Survey Program
Discovery site Purple Mountain Obs.
Discovery date6 February 2008
Designations
2012 DR30
  • 2012 DR30
  • 2009 FW54
Orbital characteristics [2] [a]
Epoch 27 April 2019 (JD  2458600.5)
Uncertainty parameter 1
Observation arc 14.72  yr (5,375 d)
Aphelion 3192  AU
2049 AU (barycentric)
Perihelion 14.5 AU
1603.44 AU
1032 AU (barycentric)
Eccentricity 0.9909
64207 yr
33100 yr (barycentric)
0.0453°
0° 0m 0s / day
Inclination 77.986°
341.48°
≈ 16 March 2011 [6]
195.57°
Jupiter  MOID 9.311 AU
Saturn  MOID 5.45 AU [1]
Uranus  MOID 3.32 AU [1]
TJupiter 0.9860
Physical characteristics
19.9 [7]
7.1 [2] [1]

    (668643) 2012 DR30 is a trans-Neptunian object and centaur with an extremely eccentric orbit that brings it from inner Oort cloud, the outermost region of the Solar System. It was discovered on 6 February 2008 by astronomers at Purple Mountain Observatory in Nanking, China. [1] It measures approximately 188 kilometers (120 miles) in diameter.

    Contents

    Description

    Using an epoch of February 2017, it has the second-largest heliocentric semi-major axis of a minor planet not detected outgassing like a comet. [8] ( 2014 FE72 has a larger heliocentric semi-major axis.) 2012 DR30 does have a barycentric semi-major axis of 1032  AU. [9] [a] For the epoch of July 2018 2012 DR30 will have its largest heliocentric semi-major axis of 1644 AU.

    Orbital evolution
    Year [a]
    (epoch)    		Barycentric
    Aphelion (Q)
    (AU)    		Orbital
    period
    years
    1950200032000
    2050204933100

    2012 DR30 passed 5.7 AU from Saturn in February 2009 and came to perihelion in March 2011 at a distance of 14.5 AU from the Sun (inside the orbit of Uranus). [2] In 2018, it will move from 18.2 AU to 19.1 AU from the Sun. [7] It comes to opposition in late March. With an absolute magnitude (H) of 7.1, [1] the object has a published diameter of 185 and 188 kilometers, respectively. [4] [5]

    With an observation arc of 14.7 years, [2] it has a well constrained orbit. It will not be 50 AU from the Sun until 2047. After leaving the planetary region of the Solar System, 2012 DR30 will have a barycentric aphelion of 2049 AU with an orbital period of 33100 years. [a] In a 10 million year integration of the orbit, the nominal (best-fit) orbit and both 3-sigma clones remain outside 12.2 AU (qmin) from the Sun. [3] Summary of barycentric orbital parameters are:

    Archived data from the JPL SBDB and MPC. [b] [c]

    Comparison

    The orbits of Sedna, 2012 VP113, Leleakuhonua, and other very distant objects along with the predicted orbit of Planet Nine. The three sednoids (pink) along with the red-colored extreme trans-Neptunian object (eTNO) orbits are suspected to be aligned with the hypothetical Planet Nine while the blue-colored eTNO orbits are anti-aligned. The highly elongated orbits colored brown include centaurs and damocloids with large aphelion distances over 200 AU. Distant object orbits + Planet Nine.png
    The orbits of Sedna, 2012 VP113 , Leleākūhonua, and other very distant objects along with the predicted orbit of Planet Nine. The three sednoids (pink) along with the red-colored extreme trans-Neptunian object (eTNO) orbits are suspected to be aligned with the hypothetical Planet Nine while the blue-colored eTNO orbits are anti-aligned. The highly elongated orbits colored brown include centaurs and damocloids with large aphelion distances over 200 AU.

    See also

    Notes

    1. 1 2 3 4 5 6 7 Given the orbital eccentricity of this object, different epochs can generate quite different heliocentric unperturbed two-body best-fit solutions to the semi-major axis and orbital period. For objects at such high eccentricity, the Sun's barycenter is more stable than heliocentric coordinates. [10] Using JPL Horizons, the barycentric semi-major axis is approximately 1032 AU. [9]
    2. ↑ Archived JPL Small-Body Database Browser: (2012 DR30) from 15 October 2014.
    3. ↑ Archived MPC object data for 2012 DR30 (2009 FW54) from 12 July 2013.

    References

    1. 1 2 3 4 5 6 7 "2012 DR30". Minor Planet Center. Archived from the original on 15 February 2017. Retrieved 19 November 2018.
    2. 1 2 3 4 5 "JPL Small-Body Database Browser: (2012 DR30)" (2014-12-17 last obs.). Jet Propulsion Laboratory. Archived from the original on 27 July 2020. Retrieved 19 November 2018.
    3. 1 2 Marc W. Buie. "Orbit Fit and Astrometric record for 12DR30". SwRI – Space Science Department. Archived from the original on 5 February 2016. Retrieved 1 February 2016.
    4. 1 2 3 4 Kiss, Cs.; Szabó, Gy.; Horner, J.; Conn, B. C.; Müller, T. G.; Vilenius, E.; et al. (July 2013). "A portrait of the extreme solar system object 2012 DR30". Astronomy and Astrophysics. 555: 13. arXiv: 1304.7112 . Bibcode:2013A&A...555A...3K. doi:10.1051/0004-6361/201321147. S2CID   54021504.
    5. 1 2 3 4 5 6 Johnston, Wm. Robert (7 October 2018). "List of Known Trans-Neptunian Objects". Johnston's Archive. Archived from the original on 23 October 2019. Retrieved 19 November 2018.
    6. ↑ JPL Horizons Archived 28 November 2020 at the Wayback Machine Observer Location: @sun
    7. 1 2 "AstDyS 2012DR30 Ephemerides". Department of Mathematics, University of Pisa, Italy. Archived from the original on 3 May 2024. Retrieved 14 February 2017. (Distance to Sun [R] from first day of 2016 to first day of 2020. Assuming average apparent magnitude for 2017.)
    8. ↑ "JPL Small-Body Database Search Engine: Asteroids and a > 100 (AU)". JPL Solar System Dynamics. Archived from the original on 29 November 2020. Retrieved 15 October 2014.
    9. 1 2 Horizons output. "Barycentric Osculating Orbital Elements for 2012 DR30". Archived from the original on 28 November 2020. Retrieved 6 March 2014. (Solution using the Solar System Barycenter and barycentric coordinates. Select Ephemeris Type:Elements and Center:@0)
    10. ↑ Kaib, Nathan A.; Becker, Andrew C.; Jones, R. Lynne; Puckett, Andrew W.; Bizyaev, Dmitry; Dilday, Benjamin; et al. (April 2009). "2006 SQ372: A Likely Long-Period Comet from the Inner Oort Cloud". The Astrophysical Journal. 695 (1): 268–275. arXiv: 0901.1690 . Bibcode:2009ApJ...695..268K. doi:10.1088/0004-637X/695/1/268. S2CID   16987581.
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