3782 Celle

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3782 Celle
Discovery [1]
Discovered byP. Jensen
Discovery siteBrorfelde Obs.
Discovery date3 October 1986
Designations
MPC designation(3782) Celle
Named after
Celle (German city)[1]
1986 TE · 1970 HD
1972 YP · 1973 AV
1978 NH2 · 1982 OB
1985 GR1
main-belt[1][2] · (inner)
Vesta[3][4]
Orbital characteristics[2]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc47.74 yr (17,437 d)
Aphelion2.6414 AU
Perihelion2.1888 AU
2.4151 AU
Eccentricity0.0937
3.75 yr (1,371 d)
247.56°
0° 15m 45.36s / day
Inclination5.2493°
271.35°
334.33°
Known satellites1 (D: 2.34 km; P:36.57 h)[5][6]
Physical characteristics
Mean diameter
5.924±0.230 km[7][8]
6.35 km (calculated)[3]
6.50±0.49 km[9]
6.6±0.7 km[10]
Mean density
2.2±0.4 g/cm3 (binary)[11]
3.8389±0.0007 h[12]
3.840±0.001 h[13]
3.840±0.0012 h[14]
3.84 h[11]
3.84 h[6]
0.232±0.09[10]
0.418±0.072[9]
0.4 (assumed)[3]
0.5033±0.0778[8]
SMASS = V[2][3] · V[15]
V–I = 0.880±0.050[10]
12.50[8][9]
12.537±0.003 (R)[14]
12.6[2][3]
13.12±0.12[10]
13.15±1.41[15]

3782 Celle, provisional designation 1986 TE, is a bright Vestian asteroid and asynchronous binary system from the inner regions of the asteroid belt, approximately 6.5 kilometers (4 miles) in diameter. It was discovered on 3 October 1986, by Danish astronomer Poul Jensen at the Brorfelde Observatory in Denmark and named after the German city of Celle.[1] The V-type asteroid has a rotation period of 3.84 hours.[3] The discovery of its 2.3-kilometer minor-planet moon was announced in 2003.[5][6]

Orbit and classification[edit]

Celle is a core member of the Vesta family (401), one of the largest families in main belt.[3][4] Vestian asteroids have a composition akin to cumulate eucrites (HED meteorites) and are thought to have originated deep within 4 Vesta's crust, possibly from the Rheasilvia crater, a large impact crater on its southern hemisphere near the South pole, formed as a result of a subcatastrophic collision. Vesta is the main belt's second-largest and second-most-massive body after Ceres.[16][17]

Celle orbits the Sun in the inner asteroid belt at a distance of 2.2–2.6 AU once every 3 years and 9 months (1,371 days; semi-major axis of 2.42 AU). Its orbit has an eccentricity of 0.09 and an inclination of 5° with respect to the ecliptic.[2] The body's observation arc begins with its first observations as 1970 HD at Crimea–Nauchnij in April 1970, about 16 years prior to its official discovery observation at Brorfelde.[1]

Physical characteristics[edit]

Celle is a bright V-type asteroid in the SMASS classification and according to the characterization made by the Pan-STARRS survey.[2][3][15] This is also in line with the overall spectral type determined for Vestian asteroids.[16]:23

Rotation period[edit]

Several rotational lightcurves of Celle have been obtained from photometric observations since 2001.[6][12][13][14][11] Analysis of the best-rated lightcurves gave a rotation period of 3.84 hours with a brightness amplitude between 0.11 and 0.17 magnitude (U=2/3-/3/3).[3]

Diameter and albedo[edit]

According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Celle measures between 5.924 and 6.6 kilometers in diameter and its surface has an albedo between 0.232 and 0.5033.[7][8][9][10]

The Collaborative Asteroid Lightcurve Link assumes a high albedo of 0.4 and calculates a diameter of 6.35 kilometers based on an absolute magnitude of 12.6.[3]

Satellite[edit]

Between September 2001, and February 2003, photometric observations of Celle were obtained with the 1.8-meter Vatican Advanced Technology Telescope on Mount Graham, Arizona, by American astronomers William Ryan at New Mexico Tech and NMHU in collaboration with Carlos Martinez and Lacey Stewart as part of a larger survey.[6]

The mutual occultation events revealed that Celle is an asynchronous binary asteroid with a minor-planet moon orbiting it every 36.57 hours (1.52 days) at an average distance of 18±1 km. The discovery was announced on 3 May 2003.[6] The satellite measures approximately 2.34±0.11 km or 43% the size of its primary. A combined bulk density of 2.2±0.4 g/cm3 was modeled for the likely basaltic bodies.[5][11]

Naming[edit]

This minor planet was named after the German city of Celle on the occasion of its 700th anniversary. Celle is twinned with the Danish town of Holbæk, where the discovering Brorfelde Observatory is located.[1] The official naming citation was published by the Minor Planet Center on 18 February 1992 (M.P.C. 19693).[18]

References[edit]

  1. ^ a b c d e f "3782 Celle (1986 TE)". Minor Planet Center. Retrieved 1 May 2018.
  2. ^ a b c d e f "JPL Small-Body Database Browser: 3782 Celle (1986 TE)" (2018-01-23 last obs.). Jet Propulsion Laboratory. Retrieved 1 May 2018.
  3. ^ a b c d e f g h i j "LCDB Data for (3782) Celle". Asteroid Lightcurve Database (LCDB). Retrieved 1 May 2018.
  4. ^ a b "Small Bodies Data Ferret". Nesvorny HCM Asteroid Families V3.0. Retrieved 1 May 2018.
  5. ^ a b c Johnston, Wm. Robert (21 September 2014). "Asteroids with Satellites Database – (3782) Celle". Johnston's Archive. Retrieved 1 May 2018.
  6. ^ a b c d e f Ryan, W. H.; Ryan, E. V.; Martinez, C. T.; Stewart, L. (May 2003). "(3782) Celle". IAU Circ. (8128). Bibcode:2003IAUC.8128....2R. Retrieved 1 May 2018.
  7. ^ a b Masiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Dailey, J.; et al. (November 2011). "Main Belt Asteroids with WISE/NEOWISE. I. Preliminary Albedos and Diameters". The Astrophysical Journal. 741 (2): 20. arXiv:1109.4096. Bibcode:2011ApJ...741...68M. doi:10.1088/0004-637X/741/2/68. Retrieved 1 May 2018.
  8. ^ a b c d Mainzer, A.; Grav, T.; Masiero, J.; Hand, E.; Bauer, J.; Tholen, D.; et al. (November 2011). "NEOWISE Studies of Spectrophotometrically Classified Asteroids: Preliminary Results" (PDF). The Astrophysical Journal. 741 (2): 25. arXiv:1109.6407. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. Retrieved 1 May 2018.
  9. ^ a b c d 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" (PDF). The Astrophysical Journal Letters. 759 (1): 5. arXiv:1209.5794. Bibcode:2012ApJ...759L...8M. doi:10.1088/2041-8205/759/1/L8. Retrieved 1 May 2018.
  10. ^ a b c d e Marchis, F.; Enriquez, J. E.; Emery, J. P.; Mueller, M.; Baek, M.; Pollock, J.; et al. (November 2012). "Multiple asteroid systems: Dimensions and thermal properties from Spitzer Space Telescope and ground-based observations". Icarus. 221 (2): 1130–1161. arXiv:1604.05384. Bibcode:2012Icar..221.1130M. doi:10.1016/j.icarus.2012.09.013. Retrieved 1 May 2018.
  11. ^ a b c d Ryan, W. H.; Ryan, E. V.; Martinez, C. T. (October 2004). "3782 Celle: Discovery of a binary system within the Vesta family of asteroids". Planetary and Space Science. 52 (12): 1093–1101. Bibcode:2004P&SS...52.1093R. doi:10.1016/j.pss.2004.07.006. Retrieved 1 May 2018.
  12. ^ a b Bowens-Rubin, Rachel; Henderson, Phoebe (January 2014). "Lightcurve Results for 899 Jokaste and 3782 Celle from Wallace Astrophysical Observatory". The Minor Planet Bulletin. 41 (1): 58–59. Bibcode:2014MPBu...41...58B. ISSN 1052-8091. Retrieved 1 May 2018.
  13. ^ a b Oey, Julian; Williams, Hasen; Groom, Roger; Pray, Donald; Benishek, Vladimir (July 2017). "Lightcurve Analysis of Binary and Potential Binary Asteroids in 2015". The Minor Planet Bulletin. 44 (3): 193–199. Bibcode:2017MPBu...44..193O. ISSN 1052-8091. Retrieved 1 May 2018.
  14. ^ a b c Waszczak, Adam; Chang, Chan-Kao; Ofek, Eran O.; Laher, Russ; Masci, Frank; Levitan, David; et al. (September 2015). "Asteroid Light Curves from the Palomar Transient Factory Survey: Rotation Periods and Phase Functions from Sparse Photometry" (PDF). The Astronomical Journal. 150 (3): 35. arXiv:1504.04041. Bibcode:2015AJ....150...75W. doi:10.1088/0004-6256/150/3/75. Retrieved 1 May 2018.
  15. ^ a b c 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" (PDF). Icarus. 261: 34–47. arXiv:1506.00762. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. Retrieved 1 May 2018.
  16. ^ a b Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families" (PDF). Asteroids IV: 297–321. arXiv:1502.01628. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. Retrieved 1 May 2018.
  17. ^ Kelley, Michael S.; Vilas, Faith; Gaffey, Michael J.; Abell, Paul A. (September 2003). "Quantified mineralogical evidence for a common origin of 1929 Kollaa with 4 Vesta and the HED meteorites". Icarus. 165 (1): 215–218. Bibcode:2003Icar..165..215K. doi:10.1016/S0019-1035(03)00149-0. Retrieved 1 May 2018.
  18. ^ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 1 May 2018.

External links[edit]