Английская Википедия:2005 VX3

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Шаблон:Infobox planet

Шаблон:Mp 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 Шаблон:Convert in diameter.[1] It has the 3rd largest known heliocentric semi-major axis and aphelion.[2] Additionally its perihelion lies within the orbit of Jupiter, which means it also has the largest orbital eccentricity of any known minor planet.

Description

Шаблон:Mp 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.[4]

Orbital evolution — Barycentric elements
Year[5]
(epoch)		 Aphelion Semimajor-axis Ref
1950 2710 AU n.a. Шаблон:Efn
2012 1914 AU n.a. Шаблон:Efn
2015 2563 AU n.a. Шаблон:Efn
2016 3235 AU n.a. Шаблон:Efn
2050 2049 AU 1026 AU Шаблон:Efn

Шаблон:Mp has a barycentric semi-major axis of ~1026 AU.[5][lower-alpha 1] Шаблон:Mpl and Шаблон:Mpl have a larger barycentric semi-major axis. The epoch of January 2016 was when Шаблон:Mp 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

Файл:Distant object orbits + Planet Nine.png
The orbits of Шаблон:Dp, Шаблон:Mpl, 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

Шаблон:Notelist

References

Шаблон:Reflist

External links

Шаблон:Trans-Neptunian objects Шаблон:Small Solar System bodies Шаблон:Authority control

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  1. ↑ Ошибка цитирования Неверный тег <ref>; для сносок johnstonsarchive-TNO-list не указан текст
  2. ↑ Ошибка цитирования Неверный тег <ref>; для сносок jpl-search не указан текст
  3. ↑ 3,0 3,1 3,2 3,3 Ошибка цитирования Неверный тег <ref>; для сносок jpldata не указан текст
  4. ↑ Ошибка цитирования Неверный тег <ref>; для сносок MPC-object не указан текст
  5. ↑ 5,0 5,1 5,2 Ошибка цитирования Неверный тег <ref>; для сносок barycenter не указан текст
  6. ↑ Ошибка цитирования Неверный тег <ref>; для сносок Kaib-2009 не указан текст


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