Astronomy:2005 VX3

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Short description: Trans-Neptunian object and retrograde damocloid on a highly eccentric, cometary-like orbit


2005 VX3
Discovery[1][2]
Discovered byMount Lemmon Srvy.
Discovery siteMount Lemmon Obs.
(first observed only)
Discovery date1 November 2005
Designations
2005 VX3
Minor planet categoryTNO[3] · damocloid[4]
unusual[5] · distant[1]
Orbital characteristics[3]
Epoch 27 April 2019 (JD 2458600.5)
Uncertainty parameter 4
Observation arc81 days
|{{{apsis}}}|helion}}1825.61 AU
|{{{apsis}}}|helion}}4.1058 AU
914.86 AU
Eccentricity0.9955
Orbital period27,672 yr
Mean anomaly0.1730°
Mean motion0° 0m 0s / day
Inclination112.22°
Longitude of ascending node255.35°
196.37°
Jupiter MOID0.8884 AU
TJupiter−0.9430
Physical characteristics
Mean diameter7 km (est.)[4]
Geometric albedo0.09 (assumed)[4]
Absolute magnitude (H)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)		 Aphelion Semimajor-axis Ref
1950 2710 AU n.a. [lower-alpha 1]
2012 1914 AU n.a. [lower-alpha 2]
2015 2563 AU n.a. [lower-alpha 3]
2016 3235 AU n.a. [lower-alpha 4]
2050 2049 AU 1026 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. ↑ 1.0 1.1 1.2 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. ↑ 2.0 2.1 Archived JPL Small-Body Database Browser: (2005 VX3) from 13 December 2012. JPL Epoch 2012 orbital solution that has aphelion (Q)=1914 AU.
  3. ↑ 3.0 3.1 Archived MPC object data for (2005 VX3) from Minor Planet Center archive of Epoch 2015-06-27 with aphelion (Q) of 2563 AU.
  4. ↑ 4.0 4.1 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. ↑ 1.0 1.1 1.2 1.3 "2005 VX3". Minor Planet Center. https://www.minorplanetcenter.net/db_search/show_object?object_id=2005+VX3. Retrieved 20 November 2018. 
  2. ↑ "MPEC 2005-V58 : 2005 VX3". IAU Minor Planet Center. 8 November 2005. https://www.minorplanetcenter.net/mpec/K05/K05V58.html. Retrieved 20 November 2018.  (K05V03X)
  3. ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 "JPL Small-Body Database Browser: (2005 VX3)". Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=3299811. Retrieved 20 November 2018. 
  4. ↑ 4.0 4.1 4.2 4.3 Johnston, Wm. Robert (7 October 2018). "List of Known Trans-Neptunian Objects". Johnston's Archive. http://www.johnstonsarchive.net/astro/tnoslist.html. Retrieved 19 November 2018. 
  5. ↑ "List Of Other Unusual Objects". Minor Planet Center. 14 November 2018. https://www.minorplanetcenter.net/iau/lists/t_others.html. Retrieved 19 November 2018. 
  6. ↑ "JPL Small-Body Database Search Engine: Asteroids and a > 100 (AU)". JPL Solar System Dynamics. http://ssd.jpl.nasa.gov/sbdb_query.cgi?obj_group=all;obj_kind=ast;obj_numbered=all;OBJ_field=0;ORB_field=0;c1_group=ORB;c1_item=Bh;c1_op=%3E;c1_value=100;table_format=HTML;max_rows=100;format_option=comp;c_fields=AcBhBgBjBiBnBsCjCpAiCkBe;.cgifields=format_option;.cgifields=ast_orbit_class;.cgifields=table_format;.cgifields=obj_kind;.cgifields=obj_group;.cgifields=obj_numbered;.cgifields=com_orbit_class&query=1&c_sort=BhD. Retrieved 2014-03-06.  (Epoch defined at will change every 6 months or so)
  7. ↑ 7.0 7.1 7.2 Horizons output. "Barycentric Osculating Orbital Elements for 2005 VX3". http://ssd.jpl.nasa.gov/horizons.cgi?find_body=1&body_group=sb&sstr=2005VX3. 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. doi:10.1088/0004-637X/695/1/268. Bibcode: 2009ApJ...695..268K. 

External links



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