Sednoid

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The orbits of the three known sednoids with Neptune's 30 AU circular orbit in blue.
The apparent magnitudes of the three known sednoids.
Discovery image of Sedna, the eponymous and first known sednoid

A sednoid is a

Kuiper cliff at 47.8 AU. The consensus among astronomers is that there are only three objects that are known from this population: 90377 Sedna, 2012 VP113, and 541132 Leleākūhonua (2015 TG387).[1] All three have perihelia greater than 60 AU.[2] These objects lie outside an apparently nearly empty gap in the Solar System and have no significant interaction with the planets. They are usually grouped with the detached objects. Some astronomers[3] consider the sednoids to be inner Oort cloud objects (OCOs), though the inner Oort cloud
, or Hills cloud, was originally predicted to lie beyond 2,000 AU, beyond the aphelia of the three known sednoids.

One attempt at a precise definition of sednoids is any body with a

semi-major axis greater than 150 AU.[4][5]
However, this definition applies to objects such as 2013 SY99 and 2021 RR205,[6] which have perihelia beyond 50 AU and semi-major axes over 700 AU. Despite this, these objects are thought to not belong to the sednoids, but rather to the same dynamical class as 474640 Alicanto, 2014 SR349 and 2010 GB174.[7][1]

With their high eccentricities (greater than 0.8), sednoids are distinguished from the high-perihelion objects with moderate eccentricities that are in a stable resonance with Neptune, namely 2015 KQ174, 2015 FJ345, (612911) 2004 XR190 ("Buffy"), 2014 FC72 and 2014 FZ71.[8]

Unexplained orbits

The sednoids' orbits cannot be explained by perturbations from the giant planets,[9] nor by interaction with the galactic tides.[4] If they formed in their current locations, their orbits must originally have been circular; otherwise accretion (the coalescence of smaller bodies into larger ones) would not have been possible because the large relative velocities between planetesimals would have been too disruptive.[10] Their present elliptical orbits can be explained by several hypotheses:

  1. These objects could have had their orbits and perihelion distances "lifted" by the passage of a nearby star when the Sun was still embedded in its birth star cluster.[11][12]
  2. Their orbits could have been disrupted by an as-yet-unknown planet-sized body beyond the Kuiper belt such as the hypothesized Planet Nine.[13][14]
  3. They could have been captured from around passing stars, most likely in the Sun's birth cluster.[9][15]

Known members

Sednoids and sednoid candidates[2][16]
Number Name Diameter
(km) 		Perihelion (AU)
Semimajor axis
(AU) 		Aphelion (AU) Heliocentric
distance (AU) 		Argument of perihelion (°) Year discovered (precovered)
90377 Sedna 995 ± 80 76.06 506 937 85.1 311.38 2003 (1990)
— 2012 VP113 300–1000[17] 80.50 271.5 462 83.65 293.78 2012 (2011)
541132 Leleākūhonua 220[18] 65.16 1085 2126 77.69 118.17 2015 (none)
Orbits and positions of three known sednoids (labeled in pink) and various other extreme trans-Neptunian objects as of 2021

The first three known sednoids, like all of the more extreme detached objects (objects with semi-major axes > 150 AU and perihelia > 30 AU; the orbit of

observational bias and is unexpected, because interaction with the giant planets should have randomized their arguments of perihelion (ω),[4] with precession periods between 40 Myr and 650 Myr and 1.5 Gyr for Sedna.[15] This suggests that one[4] or more[19] undiscovered massive perturbers may exist in the outer Solar System. A super-Earth at 250 AU would cause these objects to librate around ω = 0°±60° for billions of years. There are multiple possible configurations and a low-albedo super-Earth at that distance would have an apparent magnitude below the current all-sky-survey detection limits. This hypothetical super-Earth has been dubbed Planet Nine. Larger, more-distant perturbers would also be too faint to be detected.[4]

As of 2016[update],[

2004 XR190, 2014 FC72, and 2014 FZ71
are near the limit of perihelion of 50 AU, but are not considered sednoids.

On 1 October 2018, Leleākūhonua, then known as 2015 TG387, was announced with perihelion of 65 AU and a semimajor axis of 1094 AU. With an aphelion over 2100 AU, it brings the object further out than Sedna.

In late 2015, V774104 was announced at the Division for Planetary Science conference as a further candidate sednoid, but its observation arc was too short to know whether its perihelion was even outside Neptune's influence.[21] The talk about V774104 was probably meant to refer to Leleākūhonua (2015 TG387) even though V774104 is the internal designation for non-sednoid 2015 TH367.

Sednoids might constitute a proper dynamical class, but they may have a heterogeneous origin; the spectral slope of 2012 VP113 is very different from that of 90377 Sedna.[22]

Malena Rice and Gregory Laughlin applied a targeted shift-stacking search algorithm to analyze data from

TESS sectors 18 and 19 looking for candidate outer Solar System objects.[23] Their search recovered known objects like Sedna and produced 17 new outer Solar System body candidates located at geocentric distances in the range 80–200 AU, that need follow-up observations with ground-based telescope resources for confirmation. Early results from a survey with the William Herschel Telescope aimed at recovering these distant TNO candidates have failed to confirm two of them.[24][25]

Theoretical population

Each of the proposed mechanisms for Sedna's extreme orbit would leave a distinct mark on the structure and dynamics of any wider population. If a trans-Neptunian planet were responsible, all such objects would share roughly the same perihelion (≈80 AU). If Sedna had been captured from another planetary system that rotated in the same direction as the Solar System, then all of its population would have orbits on relatively low inclinations and have

semi-major axes ranging from 100 to 500 AU. If it rotated in the opposite direction, then two populations would form, one with low and one with high inclinations. The perturbations from passing stars would produce a wide variety of perihelia and inclinations, each dependent on the number and angle of such encounters.[26]

Acquiring a larger sample of such objects would therefore help in determining which scenario is most likely.[27] "I call Sedna a fossil record of the earliest Solar System", said Brown in 2006. "Eventually, when other fossil records are found, Sedna will help tell us how the Sun formed and the number of stars that were close to the Sun when it formed."[28] A 2007–2008 survey by Brown, Rabinowitz and Schwamb attempted to locate another member of Sedna's hypothetical population. Although the survey was sensitive to movement out to 1,000 AU and discovered the likely dwarf planet Gonggong, it detected no new sednoids.[27] Subsequent simulations incorporating the new data suggested about 40 Sedna-sized objects probably exist in this region, with the brightest being about Eris's magnitude (−1.0).[27]

Following the discovery of Leleākūhonua, Sheppard et al. concluded that it implies a population of about 2 million Inner Oort Cloud objects larger than 40 km, with a total mass in the range of 1×1022 kg, about the mass of Pluto and several times the mass of the asteroid belt.[29]

See also

References

  1. ^
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  2. ^ a b "JPL Small-Body Database Search Engine: a > 150 (AU) and q > 50 (AU) and data-arc span > 365 (d)". JPL Solar System Dynamics. Retrieved 2014-10-15.
  3. ^ Sheppard, Scott S. "Beyond the Edge of the Solar System: The Inner Oort Cloud Population". Department of Terrestrial Magnetism, Carnegie Institution for Science. Retrieved 2014-04-17.
  4. ^
    S2CID 4393431. Archived
    (PDF) from the original on 2014-12-16.
  5. ^ Sheppard, Scott S. "Known Extreme Outer Solar System Objects". Department of Terrestrial Magnetism, Carnegie Institution for Science. Retrieved 2014-04-17.
  6. ^ Sheppard, Scott S. "Scott Sheppard Small Body Discoveries". Earth and Planets Laboratory. Carnegie Institution for Science. Retrieved 10 October 2022.
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    (PDF) on 2006-06-27. Retrieved 2008-04-02.
  10. ^ Sheppard, Scott S.; Jewitt, David (2005). "Small Bodies in the Outer Solar System" (PDF). Frank N. Bash Symposium. University of Texas at Austin. Retrieved 2008-03-25.
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  15. ^ a b Jílková, Lucie; Portegies Zwart, Simon; Pijloo, Tjibaria; Hammer, Michael (2015). "How Sedna and family were captured in a close encounter with a solar sibling". MNRAS. 453 (3): 3158–3163.
    doi:10.1093/mnras/stv1803
    .
  16. ^ "MPC list of q > 50 and a > 150". Minor Planet Center. Retrieved 1 October 2018.
  17. ^ Lakdawalla, Emily (26 March 2014). "A second Sedna! What does it mean?". Planetary Society blogs. The Planetary Society. Retrieved 12 June 2019.
  18. S2CID 219039999
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  19. doi:10.1093/mnrasl/slu084
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  20. ^ "JPL Small-Body Database Search Engine: a > 150 (AU) and q > 30 (AU) and data-arc span > 365 (d)". JPL Solar System Dynamics. Retrieved 2016-02-08.
  21. S2CID 123763943
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  22. doi:10.1093/mnrasl/slx003
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  23. S2CID 225075671
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  24. doi:10.1093/mnrasl/slac036.{{cite journal}}: CS1 maint: date and year (link
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  25. ^ "Distant Trans-Neptunian Object Candidates: Fainter Than Predicted or False Positives?". 20 May 2022.
  26. ^ Schwamb, Megan E. (2007). "Searching for Sedna's Sisters: Exploring the inner Oort cloud" (PDF). None. Caltech. Archived from the original (PDF) on 2013-05-12. Retrieved 2010-08-06.
  27. ^ a b c Schwamb, Megan E.; Brown, Michael E.; Rabinowitz, David L. (2009). "A Search for Distant Solar System Bodies in the Region of Sedna". The Astrophysical Journal Letters. 694 (1): L45–L48.
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  28. ^ Fussman, Cal (2006). "The Man Who Finds Planets". Discover. Archived from the original on 16 June 2010. Retrieved 2010-05-22.
  29. S2CID 119071596
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External links


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