2012 DR30

2012 DR30
Discovery [1][2][3]
Discovered by Spacewatch
Discovery site Kitt Peak
Discovery date 31 March 2009
Designations
MPC designation 2012 DR30
2009 FW54
Distant [2] · TNO [1]
centaur [4][5]
Damocloid
Orbital characteristics [1]
Epoch 16 February 2017 (JD 2457800.5)[lower-alpha 1]
Uncertainty parameter 0
Observation arc 14.72 yr (5,375 days)
Aphelion 3070 AU
2049 AU (barycentric)[lower-alpha 1]
Perihelion 14.559 AU
1542 AU
1032 AU (barycentric)[lower-alpha 1]
Eccentricity 0.9906
60,579 yr
33100 yr (barycentric)[lower-alpha 1]
0.0350°
0° 0m 0s / day
Inclination 77.960°
341.40°
195.50°
Jupiter MOID 9.305 AU
Saturn MOID 5.46 AU[2]
Uranus MOID 3.41 AU[2]
TJupiter 0.988
Physical characteristics
Dimensions 185 km[5]
~0.08[5]
B–V = 1.10[1]
19.9[6]
7.1[1][2]

    2012 DR30 also provisionally designated 2009 FW54 is a trans-Neptunian[1] centaur[5][4] from the scattered disk/Inner Oort cloud, approximately 185–200 kilometers in diameter.[7][8]

    Using an epoch of February 2017, it has the second-largest heliocentric semi-major axis of a minor planet not detected out-gassing like a comet.[9] (2014 FE72 has a larger heliocentric semi-major axis.) 2012 DR30 does have a barycentric semi-major axis of 1032 AU.[10][lower-alpha 1] For the epoch of July 2018 2012 DR30 will have its largest heliocentric semi-major axis of 1644 AU.

    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).[1] In 2018, it will move from 18.2 AU to 19.1 AU from the Sun.[6] It comes to opposition in late March. With an absolute magnitude (H) of 7.1,[2] the object has an estimated diameter of 185 km.[5][7]

    With an observation arc of 14.7 years,[1] 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.[lower-alpha 1]

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

    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.[4]

    Summary of barycentric orbital parameters are:

    Comparison

    Sedna compared to some other very distant orbiting bodies including 2015 DB216 (orbit wrong), 2000 OO67, 2004 VN112, 2005 VX3, 2006 SQ372, 2007 TG422, 2007 DA61, 2009 MS9, 2010 GB174, 2010 NV1, 2010 BK118, 2012 DR30, 2012 VP113, 2013 BL76, 2013 AZ60, 2013 RF98, 2015 ER61

    See also

    Notes

    1. 1 2 3 4 5 6 7 8 9 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.[11] Using JPL Horizons, the barycentric semi-major axis is approximately 1032 AU.[10]

    References

    1. 1 2 3 4 5 6 7 8 "JPL Small-Body Database Browser: (2012 DR30)" (2014-12-17 last obs.). Jet Propulsion Laboratory. Archived from the original on 15 October 2014. Retrieved 14 February 2017.
    2. 1 2 3 4 5 6 "2012 DR30 (2009 FW54)". Minor Planet Center. Archived from the original on 12 July 2013. Retrieved 14 February 2017.
    3. ↑ Ernesto Guido; Giovanni Sostero & Nick Howes (2012-02-27). "Trans-Neptunian Object 2012 DR30". Remanzacco Observatory in Italy. Retrieved 2013-08-25.
    4. 1 2 3 Marc W. Buie. "Orbit Fit and Astrometric record for 12DR30". SwRI – Space Science Department. Archived from the original on 2016-02-05. Retrieved 2016-02-01.
    5. 1 2 3 4 5 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" (PDF). Astronomy and Astrophysics. 555: 13. arXiv:1304.7112. Bibcode:2013A&A...555A...3K. doi:10.1051/0004-6361/201321147. Retrieved 15 February 2017.
    6. 1 2 "AstDyS 2012DR30 Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 2017-02-14. (Distance to Sun [R] from first day of 2016 to first day of 2020. Assuming average apparent magnitude for 2017.)
    7. 1 2 Ian Musgrave (1 March 2012). "2012 DR30, no, it's not a comet, it's 2009 FW54". itelescope.net. Archived from the original on 11 December 2014. Retrieved 25 August 2013.
    8. ↑ 2012 DR30 - Ein Transneptun mit ungewöhnlicher Bahn
    9. ↑ "JPL Small-Body Database Search Engine: Asteroids and a > 100 (AU)". JPL Solar System Dynamics. Retrieved 2014-10-15.
    10. 1 2 Horizons output. "Barycentric Osculating Orbital Elements for 2012 DR30". Retrieved 2014-03-06. (Solution using the Solar System Barycenter and barycentric coordinates. Select Ephemeris Type:Elements and Center:@0)
    11. ↑ 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" (PDF). The Astrophysical Journal. 695 (1): 268–275. arXiv:0901.1690. Bibcode:2009ApJ...695..268K. doi:10.1088/0004-637X/695/1/268. Retrieved 15 February 2017.

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