(89830) 2002 CE
Discovery[1]
Discovered byLINEAR
Discovery siteLincoln Lab's ETS
Discovery date1 February 2002
Designations
(89830) 2002 CE
2002 CE
Amor · NEO · PHA[1][2]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc34.91 yr (12,752 days)
Aphelion3.1314 AU
Perihelion1.0234 AU
2.0774 AU
Eccentricity0.5074
2.99 yr (1,094 days)
117.79°
0° 19m 45.12s / day
Inclination43.701°
19.934°
5.7062°
Earth MOID0.0277 AU · 10.8 LD
Physical characteristics
Mean diameter
3.11 km (calculated)[3]
5.067±2.155 km[4]
2.6149±0.0008 h[a]
0.079±0.075[4]
0.20 (assumed)[3]
S[3][5]
14.80±0.3[4] · 14.9[1][2][3] · 15.67±0.27[6]

(89830) 2002 CE (provisional designation 2002 CE), is a stony asteroid, classified as near-Earth object and potentially hazardous asteroid of the Amor group, approximately 3.1 kilometers in diameter. It was discovered on 1 February 2002, by astronomers of the LINEAR program at Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the United States.[2] This asteroid is one of the largest potentially hazardous asteroid known to exist.[7]

Orbit and classification

2002 CE is a member of the dynamical Amor group, which are Mars-crossing asteroids that approach the orbit of Earth from beyond, but do not cross it.[1][2]

It orbits the Sun at a distance of 1.0–3.1 AU once every 2 years and 12 months (1,094 days; semi-major axis of 2.08 AU). Its orbit has a high eccentricity of 0.51 and an inclination of 44° with respect to the ecliptic.[1]

The body's observation arc begins with a precovery from the Digitized Sky Survey taken at the Siding Spring Observatory, Australia, in May 1982, nearly 20 years prior to its official discovery observation at Socorro.[2]

Close approaches

With an absolute magnitude of 14.9, 2002 CE is one of the brightest and largest known potentially hazardous asteroid (see PHA-list).[7] It has an Earth minimum orbital intersection distance of 0.0277 AU (4,140,000 km), which corresponds to 10.8 lunar distances.[1]

Physical characteristics

2002 CE has been characterized as a common, stony S-type asteroid by astronomers conducting spectroscopic observations using the New Technology Telescope at La Silla, Chile, and the 2.2-meter telescope of the Calar Alto Observatory in Spain.[5]: 6 

Rotation period

In October 2004, a rotational lightcurve of 2002 CE was obtained from photometric observations by Czech astronomer Petr Pravec at the Ondřejov Observatory. Lightcurve analysis gave a rotation period of 2.6149 hours with a low brightness amplitude of 0.09 magnitude (U=2-). Several longer periods are also possible.[a]

Diameter and albedo

According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, 2002 CE measures 5.067 kilometers in diameter and its surface has a low albedo of 0.079.[4] Conversely, the Collaborative Asteroid Lightcurve Link assumes a stony standard albedo of 0.20 and calculates a smaller diameter of 3.11 kilometers based on an absolute magnitude of 14.9.[3]

Numbering and naming

This minor planet was numbered by the Minor Planet Center on 30 August 2004.[8] As of 2018, it has not been named.[2]

Notes

  1. ^ a b Pravec (2004) web: rotation period 2.6149±0.0008 hours with a brightness amplitude of 0.09 mag. Summary figures for (89830) 2002 CE at the LCEB and Pravec, P.; Wolf, M.; Sarounova, L. (2004). Quality Code of 2−. Observation period: 11–23 October 2004. Observer's comment (Pravec): several longer periods are also possible (see Ondrejov data)

References

  1. ^ a b c d e f g "JPL Small-Body Database Browser: 89830 (2002 CE)" (2017-04-23 last obs.). Jet Propulsion Laboratory. Retrieved 17 January 2018.
  2. ^ a b c d e f "89830 (2002 CE)". Minor Planet Center. Retrieved 17 January 2018.
  3. ^ a b c d e "LCDB Data for (89830)". Asteroid Lightcurve Database (LCDB). Retrieved 17 January 2018.
  4. ^ a b c d Mainzer, A.; Grav, T.; Masiero, J.; Bauer, J.; Cutri, R. M.; McMillan, R. S.; et al. (November 2012). "Physical Parameters of Asteroids Estimated from the WISE 3-Band Data and NEOWISE Post-Cryogenic Survey". The Astrophysical Journal Letters. 760 (1): 6. arXiv:1210.0502. Bibcode:2012ApJ...760L..12M. doi:10.1088/2041-8205/760/1/L12. S2CID 41459166.
  5. ^ a b Sanchez, Juan A.; Michelsen, René; Reddy, Vishnu; Nathues, Andreas (July 2013). "Surface composition and taxonomic classification of a group of near-Earth and Mars-crossing asteroids". Icarus. 225 (1): 131–140. arXiv:1302.4449. Bibcode:2013Icar..225..131S. doi:10.1016/j.icarus.2013.02.036. S2CID 119207812.
  6. ^ Veres, Peter; Jedicke, Robert; Fitzsimmons, Alan; Denneau, Larry; Granvik, Mikael; Bolin, Bryce; et al. (November 2015). "Absolute magnitudes and slope parameters for 250,000 asteroids observed by Pan-STARRS PS1 - Preliminary results". Icarus. 261: 34–47. arXiv:1506.00762. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. S2CID 53493339.
  7. ^ a b "List of the Potentially Hazardous Asteroids (PHAs)". Minor Planet Center. Retrieved 17 January 2018.
  8. ^ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 24 February 2018.

External links

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