2005 VX3
Discovery[1][2]
Discovered byMount Lemmon Srvy.
Discovery siteMount Lemmon Obs.
(first observed only)
Discovery date1 November 2005
Designations
2005 VX3
TNO[3] · damocloid[4]
unusual[5] · distant[1]
Orbital characteristics[3]
Epoch 27 April 2019 (JD 2458600.5)
Uncertainty parameter 4
Observation arc81 days
Aphelion1825.61 AU
Perihelion4.1058 AU
914.86 AU
Eccentricity0.9955
27,672 yr
0.1730°
0° 0m 0s / day
Inclination112.22°
255.35°
196.37°
Jupiter MOID0.8884 AU
TJupiter−0.9430
Physical characteristics
Mean diameter
7 km (est.)[4]
0.09 (assumed)[4]
14.1[1][3]

    2005 VX3 is trans-Neptunian object and retrograde damocloid on a highly eccentric, cometary-like orbit. It was first observed on 1 November 2005, by astronomers with the Mount Lemmon Survey at the Mount Lemmon Observatory in Arizona, United States. The unusual object measures approximately 7 kilometers (4 miles) in diameter.[4] It has the 3rd largest known heliocentric semi-major axis and aphelion.[6] Additionally its perihelion lies within the orbit of Jupiter, which means it also has the largest orbital eccentricity of any known minor planet.

    Description

    2005 VX3 orbits the Sun at a distance of 4.1–1,826 AU once every 27,672 years (semi-major axis of 915 AU). Its orbit has an eccentricity of 0.9955 and an inclination of 112° with respect to the ecliptic. It belongs to the dynamical group of damocloids due to its retrograde orbit and its low Tisserand parameter (TJupiter of −0.9430).[3] It is a Jupiter-, Saturn-, Uranus-, and Neptune-crosser. The body's observation arc begins with its first observation by the Mount Lemmon Survey on 1 November 2005.[1]

    Orbital evolution — Barycentric elements
    Year[7]
    (epoch)    		AphelionSemimajor-axisRef
    19502710 AUn.a.[lower-alpha 1]
    20121914 AUn.a.[lower-alpha 2]
    20152563 AUn.a.[lower-alpha 3]
    20163235 AUn.a.[lower-alpha 4]
    20502049 AU1026 AU[lower-alpha 1]

    2005 VX3 has a barycentric semi-major axis of ~1026 AU.[7][lower-alpha 1] 2014 FE72 and 2012 DR30 have a larger barycentric semi-major axis. The epoch of January 2016 was when 2005 VX3 had its largest heliocentric semi-major axis.

    The object has a short observation arc of 81 days and does not have a well constrained orbit.[3] It has not been observed since January 2006, when it came to perihelion, 4.1 AU from the Sun.[3] It may be a dormant comet that has not been seen outgassing. In the past it may have made closer approaches to the Sun that could have removed most near-surface volatiles. The current orbit crosses the ecliptic just inside Jupiter's orbit and has a Jupiter-MOID of 0.8 AU.[3]

    In 2017, it had an apparent magnitude of ~28 and was 24 AU from the Sun. It comes to opposition in mid-June. It would require one of the largest telescopes in the world for any more follow-up observations.

    Comparison

    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 against the hypothetical Planet Nine while the blue-colored eTNO orbits are 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 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 barycentric coordinates are more stable than heliocentric coordinates.[8] Using JPL Horizons, the barycentric semi-major axis is approximately 1026 AU.[7]
    2. ↑ Archived JPL Small-Body Database Browser: (2005 VX3) from 13 December 2012. JPL Epoch 2012 orbital solution that has aphelion (Q)=1914 AU.
    3. ↑ Archived MPC object data for (2005 VX3) from Minor Planet Center archive of Epoch 2015-06-27 with aphelion (Q) of 2563 AU.
    4. ↑ Archived MPC object data for (2005 VX3) from JPL Webcite archive of Epoch 2016-Jan-13 with aphelion (Q) of 3235AU.
    5. Archived MPC object data for (2005 VX3) from 8 March 2014.

    References

    1. 1 2 3 4 "2005 VX3". Minor Planet Center. Retrieved 20 November 2018.
    2. ↑ "MPEC 2005-V58 : 2005 VX3". IAU Minor Planet Center. 8 November 2005. Retrieved 20 November 2018. (K05V03X)
    3. 1 2 3 4 5 6 7 "JPL Small-Body Database Browser: (2005 VX3)" (2006-01-21 last obs.). Jet Propulsion Laboratory. Retrieved 20 November 2018.
    4. 1 2 3 4 Johnston, Wm. Robert (7 October 2018). "List of Known Trans-Neptunian Objects". Johnston's Archive. Retrieved 19 November 2018.
    5. ↑ "List Of Other Unusual Objects". Minor Planet Center. 14 November 2018. Retrieved 19 November 2018.
    6. ↑ "JPL Small-Body Database Search Engine: Asteroids and a > 100 (AU)". JPL Solar System Dynamics. Retrieved 6 March 2014. (Epoch defined at will change every 6 months or so)
    7. 1 2 3 Horizons output. "Barycentric Osculating Orbital Elements for 2005 VX3". Retrieved 6 March 2014. (Solution using the Solar System Barycenter and barycentric coordinates. Select Ephemeris Type:Elements and Center:@0)
    8. ↑ 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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