(148209) 2000 CR105

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The correct title of this article is (148209) 2000 CR105. It features superscript or subscript characters that are substituted or omitted because of technical limitations.
(148209) 2000 CR105
Discovery[2] and designation
Discovered by Marc W. Buie
Discovery date February 6, 2000
Designations
Alternative names[1] none
Minor planet
category		 E-SDO
(detached object)
Epoch April 10, 2007 (JD 2454200.5)
Aphelion 59244.037 Gm (393.8 AU)
Perihelion 6611.023 Gm (44.1 AU)
Semi-major axis 32927.530 Gm (218.9 AU)
Eccentricity 0.798
Orbital period 1183743.25 d (3240.91 a)
Average orbital speed 1.63 km/s
Mean anomaly 4.73°
Inclination 22.776°
Longitude of ascending node 128.3°
Argument of perihelion 316.7°
Dimensions 253 km[4]
Mass 1.3×1019? kg[5]
Mean density 1.6? g/cm³
Equatorial surface gravity 0.0741? m/s²
Equatorial escape velocity 0.119? km/s
Sidereal rotation
period		 ? d
Axial tilt ?°
Pole ecliptic latitude ?
Pole ecliptic longitude ?
Geometric albedo 0.10?
Temperature ~19 K
Spectral type ?
Absolute magnitude 6.1[3]

(148209) 2000 CR105, also written as (148209) 2000 CR105, is currently the fourth most distant known object in the solar system after Eris, Sedna, and Buffy.[6] It circles the sun in a highly eccentric orbit every 3240 years at an average distance of 219 astronomical units (1 AU being about equal to the mean Earth-Sun distance: roughly 150 gigametres).

2000 CR105 has a diameter of around 253 km. This small size will probably prevent it from ever qualifying as a dwarf planet.[7]

2000 CR105 and Sedna differ from other scattered disc objects in that at their perihelion distances, they are not within the gravitational influence of the planet Neptune. It is something of a mystery how these objects came to be in their current far-flung orbits. Several hypotheses have been put forward:

  • They were pulled from their original positions by a passing star.[8][9]
  • They were pulled from their original positions by a very distant and as-yet-undiscovered (albeit unlikely) giant planet.[10]
  • They were pulled from their original positions by an as-yet-undiscovered companion star orbiting the Sun. (See: Nemesis (star))[10]
  • They were captured from another planetary system during a close encounter early in the Sun's history.[8] According to Kenyon and Bromley, there is a 15% probability that a star like the Sun had an early close encounter, and a 1% probability that outer planetary exchanges would have happened.[8] 2000 CR105 is 2–3 times more likely to be a captured planetary object than Sedna.

[edit] See also

[edit] External links

[edit] References

  1. ^ [1]
  2. ^ The Asteroid Orbital Elements Database. Retrieved on 2007-07-07.
  3. ^ a b JPL Small-Body Database Browser: 148209 (2000 CR105). Retrieved on 2008-02-20.
  4. ^ List of Known Trans-Neptunian Objects. Johnston's Archive. Retrieved on 2006-12-14.
  5. ^ assume radius of 126.5 km; volume of a sphere * assume the density of Phoebe @ 1.6g/cm³ (though it could be a porous rubble pile), and you get a mass of 1.35e19 kg
  6. ^ Though some long-period comets and space probes are further.
  7. ^ Michael E. Brown. The Dwarf Planets. California Institute of Technology, Department of Geological Sciences. Retrieved on 2008-02-19.
  8. ^ a b c Kenyon, Scott J.; Benjamin C. Bromley (2 December 2004). "Stellar encounters as the origin of distant Solar System objects in highly eccentric orbits" (abstract). Nature 432: 598–602. doi:10.1038/nature03136. 
  9. ^ Morbidelli, Alessandro; Harold F. Levison (2004). "Scenarios for the Origin of the Orbits of the Trans-Neptunian Objects 2000 CR105 and 2003 VB12 (Sedna)". The Astronomical Journal '128': 2564–2576. doi:10.1086/424617.  (Original Preprint)
  10. ^ a b John J. Matese, Daniel P. Whitmire, and Jack J. Lissauer, "A Widebinary Solar Companion as a Possible Origin of Sedna-like Objects", Earth, Moon, and Planets, 97:459 (2005)
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