Sednoid

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The orbits of the Sednoids

A Sednoid is a Trans-Neptunian object that has a perihelion distance of more than 50 AU and whose major semi-axis is more than 150 AU. The Sednoids were named after the first object found with these properties - (90377) Sedna . Only three objects with these properties are currently known, 90377 Sedna, 2012 VP113 and (541132) Leleākūhonua , but many more objects with these properties are expected to exist. All three currently known objects have perihelia that are greater than 64 AU. None of these objects have any significant interaction with the planets.

Differentiation from other trans-Neptunian objects

The more precise determination of the orbit data of the trans-Neptunian object 2013 SY 99 showed that its perihelion is also slightly above 50 AU, but it is not counted among the Sednoids in the literature. This seemingly arbitrary 50 AU limit for Sednoids - the Kuiper cliff (English Kuiper cliff ) is 47 AU - has historical reasons and comes from the fact that at the time of the discovery of Sedna there were no other objects beyond the Kuiper cliff and the authors of corresponding considerations may have used the next round number as a delimitation.

The same dynamic group as 2013 SY 99 also includes the Kuiper belt objects 2010 GB 174 , 2014 SR 349 and (474640) 2004 VN 112 with perihelions over 47 AU. The two Kuiper belt objects 2014 SS 349 and 2015 RX 245 of this dynamic group also have high perihelions at around 45.5 AU.

Origin of the unusual tracks

The orbits of the Sednoids can neither be explained by the interaction with the gas giants nor by disturbances of the galactic tides. It is generally believed that the Sednoids originally moved on circular orbits and that these orbits were then perturbed by a process. There are several hypotheses for the type of disorder:

  1. The sednoids could have been lifted into their elliptical inclined orbits by the close flyby of another star . Close pass-bys were likely most common during the early stages of the solar system, when it was still part of a star cluster .
  2. Their orbits could have been perturbed by an as yet undiscovered planet in the Kuiper Belt . This hypothetical planet is currently known as Planet Nine .
  3. The sednoids could also have been captured by another star as it passed close to the solar system when the sun was relatively young.

Examples

Some Sednoid objects have been suggested as members of the hypothetical Hills cloud .

Orbit parameters of highly extreme trans-Neptunian objects with perihelias greater than 30 AU and major semi-axes greater than 250 AU Note: Data taken from MPC, the information is best fits and therefore subject to great uncertainties
object Orbital period T
(years)		 Semi-axis a
(AE)		 Perihelion
q (AE)		 Aphelion
Q (AE)		 eccentricity
e		 Argument of
the periapsis
? (°)		 Inclination
i (°)		 Length of the
rise Node
Ω (°)		 Perihelion
π = ω + Ω (°)		 Absolute brightness
H (mag)
(90377) Sedna 10,590 482.24 76.08 888.39 0.84 311.6 11.9 144.4 96.0 1.5
(474640) 2004 VN 112 5,602 315.41 47.31 583.51 0.85 326.9 25.6 66.0 32.9 6.5
(523622) 2007 TG 422 10.165 469.26 35.55 902.96 0.92 285.6 18.6 112.9 38.5 6.5
2010 GB 174 6,824 359.75 48.79 670.72 0.86 347.7 21.6 130.8 118.5 6.5
2012 VP 113 ("Biden") 4.106 256.40 80.44 432.37 0.69 293.6 24.1 90.7 24.3 4.0
2013 FT 28 5,558 313.77 43.52 584.02 0.86 40.3 17.3 217.8 258.1 6.7
2013 RF 98 6,556 350.30 36.08 664.52 0.90 311.7 29.6 67.6 19.3 8.7
2013 SY 99 ("uo3l91") 17,604 676.71 49.96 1,303.45 0.93 32.3 4.2 29.5 61.8 6.7
2014 FE 72 101.195 2,171.57 36.28 4,306.86 0.98 134.3 20.6 336.8 111.1 6.1
2014 SR 349 5,064 294.90 47.65 542.14 0.84 341.1 18.0 34.8 15.9 6.7
2015 GT 50 ("o5p060") 6,073 332.85 38.46 627.24 0.88 129.3 8.8 46.1 175.4 8.5
2015 KG 163 ("o5m52") 23,718 825.50 40.50 1,610.50 0.95 32.0 14.0 219.1 251.1 8.2
2015 RX 245 ("o5t52") 8,210 406.96 45.52 768.40 0.89 65.3 12.2 8.6 73.9 6.2
2015 BP 519 ("Caju") 8,932 430.48 35.14 825.81 0.92 348.4 54.1 135.2 123.6 4.4
(541132) Leleākūhonua 36,182 1,093.94 64.94 2,122.94 0.94 118.2 11.6 300.8 59.0 5.3

Individual evidence

  1. ↑ Trujillo, Chadwick A .; Sheppard, Scott S .: A Sedna-like body with a perihelion of 80 astronomical units . In: Nature . tape 507 , 2014, p. 471-474 .
  2. ↑ Michael E. Brown, Chadwick Trujillo and David Rabinowitz: Discovery of A candidate Inner Oort Cloud Planetoid. In: The Astrophysical Journal . No. 617 , 2004, pp. 645-649 ( iop.org [PDF]).
  3. ^ Brown, Michael E.: Sedna and the birth of the solar system . In: Bulletin of the American Astronomical Society . tape 36 , 2004, p. 1553 .
  4. ^ Megan E. Schwamb, Michael E. Brown, and David L. Rabinowitz: A Search for Distant Solar System Bodies in the Region of Sedna . In: The Astrophysical Journal . No. 694 , 2009, p. L45-L48 , doi : 10.1051 / 0004-6361 / 201219931 ( caltech.edu [PDF]).
  5. ↑ Michele T. Bannister, Cory Shankman, Kathryn Volk et al .: OSSOS: V. Diffusion in the orbit of a high-perihelion distant Solar System object. In: The Astrophysical Journal . No. 153 (6) , 2017, doi : 10.3847 / 1538-3881 / aa6db5 , arxiv : 1704.01952 .
  6. ^ Chadwick A. Trujillo and Michael E. Brown: The Radial Distribution of the Kuiper Belt. In: The Astrophysical Journal Letters . No. 554 (1) , 2001 ( iop.org ).
  7. ↑ Morbidelli, A., Levinson, H .: cenarios for the Origin of the Orbits of the Trans-Neptunian Objects 2000 CR105 and 2003 VB12 . In: Astronomical Journal . tape 128 , p. 2564-2576 .
  8. ↑ Pfalzner, S., Bhandare, A., Vincke, K., Lacerda, P: Outer Solar System Possibly Shaped by a Stellar Fly-by . In: The Astrophysical Journal . tape 863 , p. 45 .
  9. ↑ R GOMES, J MATESE, J LISSAUER: A distant planetary-mass solar companion may have produced distant detached objects . In: Icarus . tape 184 , no. 2 , October 2006, ISSN  0019-1035 , p. 589-601 , doi : 10.1016 / j.icarus.2006.05.026 .
  10. ↑ Lucie Jílková, Simon Portegies Zwart, Tjibaria Pijloo, Michael Hammer: How Sedna and family were captured in a close encounter with a solar sibling . In: Monthly Notices of the Royal Astronomical Society . tape 453 , no. 3 , September 3, 2015, ISSN  0035-8711 , p. 3158-3163 , doi : 10.1093 / mnras / stv1803 ( oup.com [accessed October 9, 2018]).
  11. ↑ Website of the Minor Planet Center (MPC), list of objects with q> 30 and a> 250. International Astronomical Union (IAU), accessed January 19, 2020 .