2005 VX3

Last updated

2005 VX3
Discovery [1] [2]
Discovered by Mount Lemmon Srvy.
Discovery site Mount 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 arc 81 days
Aphelion 1825.61 AU
Perihelion 4.1058 AU
914.86 AU
Eccentricity 0.9955
27,672 yr
0.1730°
0° 0m 0s / day
Inclination 112.22°
255.35°
196.37°
Jupiter  MOID 0.8884 AU
TJupiter −0.9430
Physical characteristics
7  km (est.) [4]
0.09 (assumed) [4]
14.1 [1] [3]

    2005 VX3 is a 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.

    Contents

    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)    		AphelionSemi-major axisRef
    19502710 AUn.a. [a]
    20121914 AUn.a. [b]
    20152563 AUn.a. [c]
    20163235 AUn.a. [d]
    20502049 AU1026 AU [a]

    2005 VX3 has a barycentric semi-major axis of ~1026  AU. [7] [a] 2014 FE72 and (668643) 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.[ year needed ] It would require one of the largest telescopes in the world for any more follow-up observations.

    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 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. 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 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.
    This page is based on this Wikipedia article
    Text is available under the CC BY-SA 4.0 license; additional terms may apply.
    Images, videos and audio are available under their respective licenses.