6296 Cleveland

6296 Cleveland
Discovery [1]
Discovered byE. F. Helin
Discovery sitePalomar Obs.
Discovery date12 July 1988
Designations
(6296) Cleveland
Named after
Cleveland [1]
(U.S. city in Ohio)
1988 NC · 1982 BL12
1993 MU
main-belt · (inner)
Hungaria [1][2] · background [3][4]
Orbital characteristics [5]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc36.10 yr (13,184 d)
Aphelion2.0081 AU
Perihelion1.7741 AU
1.8911 AU
Eccentricity0.0619
2.60 yr (950 d)
291.58°
0° 22m 44.4s / day
Inclination27.052°
111.50°
36.759°
Physical characteristics
3.179±0.167 km[6]
3.18±0.17 km[6]
3.74±0.82 km[7]
15.38±0.02 h (half period)[8]
15.65±0.04 h (half period)[9]
30.84±0.03 h[10][a]
0.28±0.11[7]
0.481±0.069[6]
E (assumed)[2]
13.90[2][6]
14.00±0.59[11]
14.20[7]
14.4[1][5]

6296 Cleveland, provisional designation 1988 NC, is a Hungaria asteroid from the innermost regions of the asteroid belt, approximately 3.5 kilometers (2.2 miles) in diameter. It was discovered on 12 July 1988, by American astronomer Eleanor Helin at the Palomar Observatory in California.[1] The presumed E-type asteroid has a long rotation period of 30.8 hours and possibly an elongated shape.[2] It was named for the city of Cleveland in the U.S. state of Ohio.[1]

Orbit and classification

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Cleveland is a Hungaria asteroid, a dynamical group that forms the innermost dense concentration of asteroids in the Solar System.[2] However it is a background asteroid and does not belong to the Hungaria family.[3][4] It orbits the Sun in the inner main-belt at a distance of 1.8–2.0 AU once every 2 years and 7 months (950 days; semi-major axis of 1.89 AU). Its orbit has an eccentricity of 0.06 and an inclination of 27° with respect to the ecliptic.[5] The body's observation arc begins with its first observation as 1982 BL12 at Crimea–Nauchnij in January 1982, more than six years prior to its official discovery observation at Palomar .[1]

Physical characteristics

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Cleveland is an assumed E-type asteroid.[2]

Rotation period

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In April 2011, a rotational lightcurve of Cleveland was obtained from photometric observations by American astronomer Brian Warner at his Palmer Divide Observatory in Colorado. Lightcurve analysis gave a rotation period of 30.84 hours with a brightness amplitude of 0.70 magnitude, indicative of a non-spherical shape (U=3).[2][10][a] While not being a slow rotator, Cleveland's period is significantly longer than for most other asteroids, which typically have periods between 2 and 20 hours. The result supersedes previous measurements that gave 15.38 and 15.65 hours, or half the period solution of the 2011 measurement (U=2/2).[8][9]

Diameter and albedo

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According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Cleveland measures between 3.179 and 3.74 kilometers in diameter and its surface has an albedo between 0.28 and 0.481.[6][7]

The Collaborative Asteroid Lightcurve Link adopts an albedo of 0.481 and a diameter of 3.18 kilometers based on an absolute magnitude of 13.9.[2]

Naming

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This minor planet was named after the U.S. city of Cleveland as a tribute to its bicentennial celebration.[1] The official naming citation was published by the Minor Planet Center on 9 September 1995 (M.P.C. 25655).[12]

Notes

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  1. ^ a b Lightcurve plot of 6296 Cleveland, Palmer Divide Observatory, B. D. Warner (2011): Rotation period 30.84±0.03 hours with a brightness amplitude of 0.70±0.03 mag. Quality code is 3. Summary figures for (6296) Cleveland at the LCDB.

References

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  1. ^ a b c d e f g h "6296 Cleveland (1988 NC)". Minor Planet Center. Retrieved 27 May 2018.
  2. ^ a b c d e f g h "LCDB Data for (6296) Cleveland". Asteroid Lightcurve Database (LCDB). Retrieved 27 May 2018.
  3. ^ a b "Asteroid 6296 Cleveland". Small Bodies Data Ferret. Retrieved 27 May 2018.
  4. ^ a b "Asteroid (6296) Cleveland". AstDyS-2, Asteroids – Dynamic Site. Retrieved 27 May 2018.
  5. ^ a b c "JPL Small-Body Database Browser: 6296 Cleveland (1988 NC)" (2018-02-27 last obs.). Jet Propulsion Laboratory. Retrieved 27 May 2018.
  6. ^ a b c d e Masiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Nugent, C.; et al. (November 2012). "Preliminary Analysis of WISE/NEOWISE 3-Band Cryogenic and Post-cryogenic Observations of Main Belt Asteroids". The Astrophysical Journal Letters. 759 (1): 5. arXiv:1209.5794. Bibcode:2012ApJ...759L...8M. doi:10.1088/2041-8205/759/1/L8.
  7. ^ a b c d Nugent, C. R.; Mainzer, A.; Masiero, J.; Bauer, J.; Cutri, R. M.; Grav, T.; et al. (December 2015). "NEOWISE Reactivation Mission Year One: Preliminary Asteroid Diameters and Albedos". The Astrophysical Journal. 814 (2): 13. arXiv:1509.02522. Bibcode:2015ApJ...814..117N. doi:10.1088/0004-637X/814/2/117.
  8. ^ a b Warner, Brian D. (December 2006). "Asteroid lightcurve analysis at the Palmer Divide Observatory - March - June 2006". The Minor Planet Bulletin. 33 (4): 85–88. Bibcode:2006MPBu...33...85W. ISSN 1052-8091.
  9. ^ a b Warner, Brian D. (September 2008). "Asteroid Lightcurve Analysis at the Palmer Divide Observatory: December 2007 - March 2008". The Minor Planet Bulletin. 35 (3): 95–98. Bibcode:2008MPBu...35...95W. ISSN 1052-8091.
  10. ^ a b Warner, Brian D. (October 2011). "Asteroid Lightcurve Analysis at the Palmer Divide Observatory: 2011 March - July". The Minor Planet Bulletin. 38 (4): 190–195. Bibcode:2011MPBu...38..190W. ISSN 1052-8091.
  11. ^ 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.
  12. ^ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 27 May 2018.
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