Английская Википедия:(308933) 2006 SQ372

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Шаблон:Mp is a trans-Neptunian object and highly eccentric centaur on a cometary-like orbit in the outer region of the Solar System, approximately Шаблон:Convert in diameter. It was discovered through the Sloan Digital Sky Survey by astronomers Andrew Becker, Andrew Puckett and Jeremy Kubica on images first taken on 27 September 2006 (with precovery images dated to 13 September 2005).

Characteristics

Файл:308933 2006 SQ 372 Orbit.png

Diagram of the orbit of Шаблон:Mp

It has a highly eccentric orbit, crossing that of Neptune near perihelion but bringing it more than 1,500 AU from the Sun at aphelion. It takes about 22,500 years to orbit the barycenter of the Solar System. The large semi-major axis makes it similar to Шаблон:Mpl- and Шаблон:Dp. With an absolute magnitude (H) of 8.1, it is estimated to be about 60 to 140 km in diameter. Michael Brown estimates that it has an albedo of 0.08 which would give a diameter of around 110 km.

The object could possibly be a comet. The discoverers hypothesize that the object could come from the Hills cloud, but other scientists like California Institute of Technology's Michael Brown also consider other possibilities, including the theory "it may have formed from debris just beyond Neptune [in the Kuiper belt] and been 'kicked' into its distant orbit by a planet like Neptune or Uranus".

Perturbation

The orbit of Шаблон:Mp currently comes closer to Neptune than any of the other giant planets. More than half of the simulations of this object show that it gets too close to either Uranus or Neptune within the next 180 million years, sending it in a currently unknown direction. This makes it difficult to classify this object as only a centaur or a scattered disc object. The Minor Planet Center, which officially catalogues all trans-Neptunian objects, lists centaurs and SDOs together. Шаблон:Mpl is another such object that blurs the two categories.

Baricentric orbital elements

• aphelion (Q) = 1570 AUШаблон:Ref label (Heliocentric 2006 AU)
• semimajor =736.67 AUШаблон:Ref label (Heliocentric 1015 AU)
• period = 22,466 yrШаблон:Ref label (Heliocentric 32,347 yr)

Given the extreme orbital eccentricity of this object, different epochs can generate quite different heliocentric unperturbed two-body best-fit solutions to the aphelion distance (maximum distance) of this object.Шаблон:Ref label With a 2005 epoch the object had an approximate period of about 22,000 years with aphelion at 1557 AU. But using a 2011 epoch shows a period of about 32,000 years with aphelion at 2006 AU. For objects at such high eccentricity, the Sun's barycentric coordinates are more stable than heliocentric coordinates. Using JPL Horizons with an observed orbital arc of only 2.9 years, the barycentric orbital elements for epoch 2008-May-14 generate a semi-major axis of 796 AU and a period of 22,466 years.

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 with the hypothetical Planet Nine while the blue-colored eTNO orbits are anti-aligned. The highly elongated orbits colored brown include centaurs and damocloids with large aphelion distances over 200 AU.

See also

• Шаблон:Mpl
• Шаблон:LoMP
• Шаблон:Mpl
• List of Solar System objects by greatest aphelion

Notes

1. Шаблон:Note label Solution using the Solar System Barycenter
2. Шаблон:Note label Read osculating orbit for more details about heliocentric unperturbed two-body solutions

External links

• Шаблон:Cite journal
• Шаблон:JPL small body