Centaur (minor planet)

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Positions of known outer Solar System objects. The centaurs are those objects (in orange) that lie generally inwards of the Kuiper belt (in green) and outside the Jupiter Trojans (pink).

Centaurs are small Solar System bodies with a semi-major axis between those of the outer planets. They have unstable orbits that cross or have crossed the orbits of one or more of the giant planets, and have dynamic lifetimes of a few million years.[1] Centaurs typically behave with characteristics of both asteroids and comets. They are named after the mythological beings that were a mixture of horse and human, centaurs. It has been estimated that there are around 44,000 centaurs in the Solar System with diameters larger than 1 km.[1]

The first centaur to be discovered was 944 Hidalgo in 1920. However, they were not recognized as a distinct population until the discovery of 2060 Chiron in 1977. The largest confirmed centaur is 10199 Chariklo, which at 260 km in diameter is as big as a mid-sized main-belt asteroid, and is known to have a system of rings. It was discovered in 1997. However, the lost centaur, 1995 SN55, may be somewhat larger.

No centaur has been photographed up close, although there is evidence that Saturn's moon Phoebe, imaged by the Cassini probe in 2004, may be a captured centaur. In addition, the Hubble Space Telescope has gleaned some information about the surface features of 8405 Asbolus.

As of 2008, three centaurs have been found to display cometary comas: Chiron, 60558 Echeclus, and 166P/NEAT. Chiron and Echeclus are therefore classified as both asteroids and comets. Other centaurs such as 52872 Okyrhoe are suspected of showing cometary activity. Any centaur that is perturbed close enough to the Sun is expected to become a comet.

Classification[edit]

The generic definition of a centaur is a small body that orbits the Sun between Jupiter and Neptune and crosses the orbits of one or more of the giant planets. Due to the inherent long-term instability of orbits in this region, even centaurs such as 2000 GM137 and 2001 XZ255, which do not currently cross the orbit of any planet, are in gradually changing orbits that will be perturbed until they start to cross the orbit of one or more of the giant planets.[1]

However, different institutions have different criteria for classifying borderline objects, based on particular values of their orbital elements:

  • The Minor Planet Center (MPC) defines centaurs as having a perihelion beyond the orbit of Jupiter and a semi-major axis less than that of Neptune.[2]
  • The Jet Propulsion Laboratory (JPL) similarly defines centaurs as having a semi-major axis, a, between those of Jupiter and Neptune (5.5 AU < a < 30.1 AU).[3]
  • In contrast, the Deep Ecliptic Survey (DES) defines centaurs using a dynamical classification scheme. These classifications are based on the simulated change in behavior of the present orbit when extended over 10 million years. The DES defines centaurs as non-resonant objects whose instantaneous (osculating) perihelia are less than the osculating semi-major axis of Neptune at any time during the simulation. This definition is intended to be synonymous with planet-crossing orbits and to suggest comparatively short lifetimes in the current orbit.[4]

The collection The Solar System Beyond Neptune (2008) uses the traditional definition of centaurs, limited to semi-major axes smaller than that of Neptune, classifying the objects on unstable orbits beyond this limit as members of the scattered disc.[5] Yet, other astronomers still prefer to define centaurs as objects that are non-resonant with a perihelion inside the orbit of Neptune that can be shown to likely cross the Hill sphere of a gas giant within the next 10 million years.[6] Thus centaurs can be thought of as inward scattered objects that interact more aggressively and scatter more quickly than typical scattered disc objects.

The JPL Small-Body Database lists 183 centaurs.[7] There are an additional 40 trans-Neptunian objects with a semi-major axis further than Neptune (a > 30.1 AU) and perihelion closer than the orbit of Uranus (q < 19 AU).[7] The Committee on Small Body Nomenclature of the International Astronomical Union has not formally weighed in on either side of the debate. Instead, it has adopted the following naming convention for such objects: befitting their centaur-like transitional orbits between TNOs and comets, "objects on unstable, non-resonant, giant-planet-crossing orbits with semimajor axes greater than Neptune's" are to be named for other hybrid and shape-shifting mythical creatures. Thus far, only the binary objects Ceto and Phorcys and Typhon and Echidna have been named according to the new policy.[8]

Other objects caught between these differences in classification methods include (44594) 1999 OX3, which has a semi-major axis of 32 AU but crosses the orbits of both Uranus and Neptune. Among the inner centaurs, 2005 VD, with a perihelion distance very near Jupiter, is listed as a centaur by both JPL and DES.

Centaurs with measured diameters listed as possible dwarf planets according to Mike Brown's website include 10199 Chariklo, 2060 Chiron, and 54598 Bienor.[9]

Orbits[edit]

Distribution[edit]

Orbits of known centaurs[note 1]

The diagram at right illustrates the orbits of all known centaurs in relation to the orbits of the planets. For selected objects, the eccentricity of the orbits is represented by red segments (extending from perihelion to aphelion).

Centaurs' orbits are characterised by a wide range of eccentricity, from highly eccentric (Pholus, Asbolus, Amicus, Nessus) to more circular (Chariklo and the Saturn-crossers: Thereus, Okyrhoe).

To illustrate the range of the orbits' parameters, a few objects with very unusual orbits are plotted in yellow on the diagram:

  • 1999 XS35 (Apollo asteroid) follows an extremely eccentric orbit (e=0.947), leading it from inside Earth's orbit (0.94 AU) to well beyond Neptune (>34 AU)
  • 2007 TB434 follows a quasi-circular orbit (e<0.026)
  • 2001 XZ255 has the lowest inclination (i<3°).
  • Damocles is among a few centaurs on orbits with extreme inclination (prograde i>70°, e.g. 2007 DA61, 2004 YH32, retrograde i<120° e.g. 2005 JT50; not shown)
  • 2004 YH32 follows such a highly inclined orbit (nearly 80°) that, while it crosses from the distance of the asteroid belt from the Sun to past the distance of Saturn, if its orbit is projected onto the plane of Jupiter's orbit, it does not even go out as far as Jupiter.

A dozen known centaurs, including Dioretsa ("asteroid" spelled backwards), follow retrograde orbits.

Changing orbits[edit]

The semi-major axis of Asbolus during the next 5500 years, using two slightly different estimates of present-day orbital elements. After the Jupiter encounter of year 4713 the two calculations diverge.[10]

Because the centaurs are not protected by orbital resonances, their orbits are unstable within a timescale of 106–107 years.[11] For example, 55576 Amycus is in an unstable orbit near the 3:4 resonance of Uranus.[1] Dynamical studies of their orbits indicate that being a centaur is probably an intermediate orbital state of objects transitioning from the Kuiper belt to the Jupiter family of short-period comets. Objects may be perturbed from the Kuiper belt, whereupon they become Neptune-crossing and interact gravitationally with that planet (see theories of origin). They then become classed as centaurs, but their orbits are chaotic, evolving relatively rapidly as the centaur makes repeated close approaches to one or more of the outer planets. Some centaurs will evolve into Jupiter-crossing orbits whereupon their perihelia may become reduced into the inner Solar System and they may be reclassified as active comets in the Jupiter family if they display cometary activity. Centaurs will thus ultimately collide with the Sun or a planet or else they may be ejected into interstellar space after a close approach to one of the planets, particularly Jupiter.

Physical characteristics[edit]

The relatively small size of centaurs precludes surface observations, but colour indices and spectra can indicate possible surface composition and can provide insight into the origin of the bodies.[11]

Colours[edit]

Colour distribution of centaurs

Centaurs display a puzzling diversity of colour that challenges any simple model of surface composition.[12] In the side-diagram, the colour indices are measures of apparent magnitude of an object through blue (B), visible (V) i.e. green-yellow and red (R) filters. The diagram illustrates these differences (in enhanced colour) for all centaurs with known colour indices. For reference, two moons: Triton and Phoebe, and planet Mars are plotted (yellow labels, size not to scale).

Centaurs appear to be grouped into two classes:

There are numerous theories to explain this colour difference, but they can be divided broadly into two categories:

  • The colour difference results from a difference in the origin and/or composition of the centaur (see origin below)
  • The colour difference reflects a different level of space-weathering from radiation and/or cometary activity.

As examples of the second category, the reddish colour of Pholus has been explained as a possible mantle of irradiated red organics, whereas Chiron has instead had its ice exposed due to its periodic cometary activity, giving it a blue/grey index. The correlation with activity and color is not certain, however, as the active centaurs span the range of colors from blue (Chiron) to red (166P/NEAT).[13] Alternatively, Pholus may have been only recently expelled from the Kuiper belt, so that surface transformation processes have not yet taken place.

Delsanti et al. suggest multiple competing processes: reddening by the radiation, and blushing by collisions.[14][15]

Spectra[edit]

The interpretation of spectra is often ambiguous, related to particle sizes and other factors, but the spectra offer an insight into surface composition. As with the colours, the observed spectra can fit a number of models of the surface.

Water ice signatures have been confirmed on a number of centaurs[11] (including 2060 Chiron, 10199 Chariklo and 5145 Pholus). In addition to the water ice signature, a number of other models have been put forward:

Comet 38P exhibits centaur-like behavior by making close approaches to Jupiter, Saturn, and Uranus between 1982 and 2067.[17]

Chiron, the only centaur with known cometary activity, appears to be the most complex. The spectra observed vary depending on the period of the observation. Water ice signature was detected during a period of low activity and disappeared during high activity.[18][19][20]

Similarities to comets[edit]

Observations of Chiron in 1988 and 1989 near its perihelion found it to display a coma (a cloud of gas and dust evaporating from its surface). It is thus now officially classified as both a comet and an asteroid, although it is far larger than a typical comet and there is some lingering controversy. Other centaurs are being monitored for comet-like activity: so far two, 60558 Echeclus, and 166P/NEAT have shown such behavior. 166P/NEAT was discovered while it exhibited a coma, and so is classified as a comet, though its orbit is that of a centaur. 60558 Echeclus was discovered without a coma but recently became active,[21] and so it is now accordingly also classified as both a comet and an asteroid.

There is no clear orbital distinction between centaurs and comets. Both 29P/Schwassmann-Wachmann and 39P/Oterma have been referred to as centaurs since they have typical centaur orbits. The comet 39P/Oterma is currently inactive and was seen to be active only before it was perturbed into a centaur orbit by Jupiter in 1963.[22] The faint comet 38P/Stephan–Oterma would probably not show a coma if it had a perihelion distance beyond Jupiter's orbit at 5 AU. By the year 2200, comet 78P/Gehrels will probably migrate outwards into a centaur-like orbit.

Theories of origin[edit]

The study of centaur development is rich in recent developments but still hampered by limited physical data. Different models have been put forward for possible origin of centaurs.

Simulations indicate that the orbit of some Kuiper-belt objects can be perturbed, resulting in the object's expulsion so that it becomes a centaur. Scattered disc objects would be dynamically the best candidates[23] for such expulsions, but their colours do not fit the bicoloured nature of the centaurs. Plutinos are a class of Kuiper-belt object that display a similar bicoloured nature, and there are suggestions that not all plutinos' orbits are as stable as initially thought, due to perturbation by Pluto.[24] Further developments are expected with more physical data on KBOs.

Notable centaurs[edit]

Well-known centaurs include:

Name Year Discoverer Half-life[1]
(forward)
Class[clarification needed]
55576 Amycus 2002 NEAT at Palomar 11.1 Myr UE
54598 Bienor 2000 Marc W. Buie et al.  ?  ?
10370 Hylonome 1995 Mauna Kea Observatory 6.3 Myr UN
10199 Chariklo 1997 Spacewatch 10.3 Myr U
8405 Asbolus 1995 Spacewatch (James V. Scotti) 0.86 Myr SN
7066 Nessus 1993 Spacewatch (David L. Rabinowitz) 4.9 Myr SE
5145 Pholus 1992 Spacewatch (David L. Rabinowitz) 1.28 Myr SN
2060 Chiron 1977 Charles T. Kowal 1.03 Myr SU
944 Hidalgo 1920 Walter Baade  ?  ?

See also[edit]

Notes[edit]

  1. ^ For the purpose of this diagram, an object is classified as a centaur if its semi-major axis lies between Jupiter and Neptune. Last update: October 2008

References[edit]

  1. ^ a b c d e Horner, J.; Evans, N.W.; Bailey, M. E. (2004). "Simulations of the Population of Centaurs I: The Bulk Statistics". Monthly Notices of the Royal Astronomical Society 354 (3): 798–810. arXiv:astro-ph/0407400. Bibcode:2004MNRAS.354..798H. doi:10.1111/j.1365-2966.2004.08240.x. 
  2. ^ "Unusual Minor Planets". Minor Planet Center. Retrieved 2010-10-25. 
  3. ^ "Orbit Classification (Centaur)". JPL Solar System Dynamics. Retrieved 2008-10-13. 
  4. ^ Elliot, J.L.; Kern, Buie, Trilling; et al. (2005). "The Deep Ecliptic Survey: A Search for Kuiper Belt Objects and Centaurs. II. Dynamical Classification, the Kuiper Belt Plane, and the Core Population". The Astronomical Journal 129 (2): 1117–1162. Bibcode:2005AJ....129.1117E. doi:10.1086/427395. Retrieved 2008-09-22. 
  5. ^ B. Gladman, B. Marsden, C. VanLaerhoven (2008). "Nomenclature in the Outer Solar System". In The Solar System Beyond Neptune, ISBN 978-0-8165-2755-7. 
  6. ^ Chaing, Eugene; Buie, Grundy, Holman; et al. (2007). "A Brief History of Transneptunian Space". Protostars and Planets V, B. Reipurth, D. Jewitt, and K. Keil (eds.), University of Arizona Press, Tucson: 895–911. arXiv:astro-ph/0601654. Bibcode:2006astro.ph..1654C. 
  7. ^ a b "JPL Small-Body Database Search Engine". JPL Solar System Dynamics. Retrieved 2010-12-27. 
  8. ^ Grundy, Will; Stansberry, J.A.; Noll, K; Stephens, D.C.; Trilling, D.E.; Kern, S.D.; Spencer, J.R.; Cruikshank, D.P.; Levison, H.F. (2007). "The orbit, mass, size, albedo, and density of (65489) Ceto/Phorcys: A tidally-evolved binary Centaur". Icarus 191 (1): 286–297. arXiv:0704.1523. Bibcode:2007Icar..191..286G. doi:10.1016/j.icarus.2007.04.004. 
  9. ^ Michael E. Brown. "How many dwarf planets are there in the outer solar system? (updates daily)". California Institute of Technology. Retrieved 2012-01-16. 
  10. ^ "Three clones of Centaur 8405 Asbolus making passes within 450Gm". Retrieved 2009-05-02.  (Solex 10)
  11. ^ a b c Jewitt, David C.; A. Delsanti (2006). "The Solar System Beyond The Planets". Solar System Update : Topical and Timely Reviews in Solar System Sciences. Springer-Praxis Ed. ISBN 3-540-26056-0.  (Preprint version (pdf))
  12. ^ M. A. Barucci, A. Doressoundiram, and D. P. Cruikshank, "Physical Characteristics of TNOs and Centaurs" (2003), available on the web (accessed 3/20/2008)
  13. ^ Bauer, J. M., Fernández, Y. R., & Meech, K. J. 2003. "An Optical Survey of the Active Centaur C/NEAT (2001 T4)", Publication of the Astronomical Society of the Pacific", 115, 981
  14. ^ Peixinho, N.; Doressoundiram, A.; Delsanti, A.; Boehnhardt, H.; Barucci, M. A.; Belskaya, I. (2003). "Reopening the TNOs Color Controversy: Centaurs Bimodality and TNOs Unimodality". Astronomy and Astrophysics 410 (3): L29–L32. arXiv:astro-ph/0309428. Bibcode:2003A&A...410L..29P. doi:10.1051/0004-6361:20031420. 
  15. ^ Hainaut & Delsanti (2002) Color of Minor Bodies in the Outer Solar System Astronomy & Astrophysics, 389, 641 datasource
  16. ^ A class of Magnesium Iron Silicates (Mg, Fe)2SiO4, common components of igneous rocks.
  17. ^ "JPL Close-Approach Data: 38P/Stephan-Oterma". 1981-04-04 last obs. Retrieved 2009-05-07.  Check date values in: |date= (help)
  18. ^ Dotto, E; Barucci, M A; De Bergh, C, Colours and composition of the centaurs, Earth, Moon, and Planets, 92, no. 1–4, pp. 157–167. (June 2003)
  19. ^ Luu, Jane X.; Jewitt, David; Trujillo, C. A. (2000). "Water Ice on 2060 Chiron and its Implications for Centaurs and Kuiper Belt Objects". The Astrophysical Journal 531 (2): L151–L154. arXiv:astro-ph/0002094. Bibcode:2000ApJ...531L.151L. doi:10.1086/312536. PMID 10688775. 
  20. ^ Fernandez, Y. R.; Jewitt, D. C.; Sheppard, S. S. (2002). "Thermal Properties of Centaurs Asbolus and Chiron". The Astronomical Journal 123 (2): 1050–1055. arXiv:astro-ph/0111395. Bibcode:2002AJ....123.1050F. doi:10.1086/338436. 
  21. ^ Y-J. Choi, P.R. Weissman, and D. Polishook (60558) 2000 EC_98, IAU Circ., 8656 (Jan. 2006), 2.
  22. ^ Mazzotta Epifani, E.; Palumbo; Capria; Cremonese;; et al. (2006). "The dust coma of the active Centaur P/2004 A1 (LONEOS): a CO-driven environment?". Astronomy & Astrophysics 460 (3): 935–944. Bibcode:2006A&A...460..935M. doi:10.1051/0004-6361:20065189. Retrieved 2009-05-08. 
  23. ^ for instance, the centaurs could be part of an "inner" scattered disc of objects perturbed inwards from the Kuiper belt [1].
  24. ^ Wan, X.-S; Huang, T.-Y. (2001). "The orbit evolution of 32 plutinos over 100 million year". Astronomy and Astrophysics 368 (2): 700–705. Bibcode:2001A&A...368..700W. doi:10.1051/0004-6361:20010056. 

External links[edit]