1275 Cimbria

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1275 Cimbria
Discovery [1]
Discovered by K. Reinmuth
Discovery site Heidelberg Obs.
Discovery date 30 November 1932
Designations
MPC designation (1275) Cimbria
Named after
Cimbri[2]
(ancient Germanic tribe)
1932 WG · 1949 QL2
A914 TG
main-belt · (middle)
Eunomia[3][4]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 84.42 yr (30,833 days)
Aphelion 3.1314 AU
Perihelion 2.2301 AU
2.6807 AU
Eccentricity 0.1681
4.39 yr (1,603 days)
143.95°
0° 13m 28.56s / day
Inclination 12.877°
188.56°
196.98°
Physical characteristics
Dimensions 18.70±4.19 km[5]
26.31±0.30 km[6]
27.622±0.500 km[7]
28.65±4.4 km[3][8]
30.94±4.26 km[9]
33.599±0.594 km[10]
5.65±0.05 h[11]
5.65454±0.00001 h[12]
5.655±0.0023 h[13]
0.0807±0.0106[10]
0.095±0.039[9]
0.1109±0.044[3][8]
0.135±0.004[6]
0.141±0.007[7]
0.25±0.13[5]
Tholen = X[1] · X[14] · M[3]
B–V = 0.698[1]
U–B = 0.304[1]
10.426±0.001 (R)[13] · 10.72[1][3][6][8][9][10] · 10.78[5] · 11.07±1.21[14]

1275 Cimbria, provisional designation 1932 WG, is a Eunomian asteroid from the central regions of the asteroid belt, approximately 27 kilometers in diameter. It was discovered on 30 November 1932, by astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory in southern Germany.[15] The asteroid was named after the Cimbri, an ancient Germanic tribe.[2]

Orbit and classification[edit]

Cimbria is a member of the Eunomia family (502),[3][4] a prominent family of typically stony asteroids and the largest one in the intermediate main belt with more than 5,000 members.[16]

The asteroid orbits the Sun in the central main-belt at a distance of 2.2–3.1 AU once every 4 years and 5 months (1,603 days). Its orbit has an eccentricity of 0.17 and an inclination of 13° with respect to the ecliptic.[1] It was first identified as A914 TG at Simeiz Observatory in October 1914. The body's observation arc begins with its official discovery observation at Heidelberg in 1932.[15]

Physical characteristics[edit]

In the Tholen classification, Cimbria is an X-type asteroid, rather than a stony S-type asteroid, which is the overall spectral type for members of the Eunomia family.[16]:23

Rotation period[edit]

In November and December 2002, two rotational lightcurves of Cimbria were obtained from photometric observations by Italian amateur astronomers Silvano Casulli, Antonio Vagnozzi, Marco Cristofanelli and Marco Paiella. Lightcurve analysis gave a well-defined rotation period of 5.65 hours with a brightness variation of 0.40 and 0.57 magnitude, respectively (U=3/3-).[11] In December 2012, astronomers at the Palomar Transient Factory in California measured a period of 5.655 hours and an amplitude of 0.26 magnitude (U=2).[13]

Poles[edit]

The asteroid's lightcurve has also been modeled using photometric data from the Lowell Photometric Database. It gave a concurring period of 5.65454 hours and determined two spin axis of (85.0°, −61.0°) and (271.0°, −31.0°) in ecliptic coordinates (λ, β).[12]

Diameter and albedo[edit]

According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Cimbria measures between 18.70 and 33.599 kilometers in diameter and its surface has an albedo between 0.0807 and 0.25.[5][6][7][8][9][10]

The Collaborative Asteroid Lightcurve Link adopts the results obtained by IRAS, that is an albedo of 0.1109 and a diameter of 28.65 kilometers based on an absolute magnitude of 10.72.[3][8]

Naming[edit]

This minor planet was named after the Cimbri, an ancient Proto-Germanic tribe that fought the Romans together with the Teutons and the Ambrones. At first victorious, they were destroyed by Gaius Marius in the Cimbrian War (113–101 BC). The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 117).[2]

References[edit]

  1. ^ a b c d e f g "JPL Small-Body Database Browser: 1275 Cimbria (1932 WG)" (2017-05-01 last obs.). Jet Propulsion Laboratory. Retrieved 28 October 2017. 
  2. ^ a b c Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (1275) Cimbria. Springer Berlin Heidelberg. p. 105. ISBN 978-3-540-00238-3. Retrieved 28 October 2017. 
  3. ^ a b c d e f g "LCDB Data for (1275) Cimbria". Asteroid Lightcurve Database (LCDB). Retrieved 28 October 2017. 
  4. ^ a b "Small Bodies Data Ferret". Nesvorny HCM Asteroid Families V3.0. Retrieved 28 October 2017. 
  5. ^ a b c d Nugent, C. R.; Mainzer, A.; Bauer, J.; Cutri, R. M.; Kramer, E. A.; Grav, T.; et al. (September 2016). "NEOWISE Reactivation Mission Year Two: Asteroid Diameters and Albedos". The Astronomical Journal. 152 (3): 12. arXiv:1606.08923Freely accessible. Bibcode:2016AJ....152...63N. doi:10.3847/0004-6256/152/3/63. Retrieved 28 October 2017. 
  6. ^ a b c d Usui, Fumihiko; Kuroda, Daisuke; Müller, Thomas G.; Hasegawa, Sunao; Ishiguro, Masateru; Ootsubo, Takafumi; et al. (October 2011). "Asteroid Catalog Using Akari: AKARI/IRC Mid-Infrared Asteroid Survey". Publications of the Astronomical Society of Japan. 63 (5): 1117–1138. Bibcode:2011PASJ...63.1117U. doi:10.1093/pasj/63.5.1117. Retrieved 28 October 2017. 
  7. ^ a b c Masiero, Joseph R.; Grav, T.; Mainzer, A. K.; Nugent, C. R.; Bauer, J. M.; Stevenson, R.; et al. (August 2014). "Main-belt Asteroids with WISE/NEOWISE: Near-infrared Albedos". The Astrophysical Journal. 791 (2): 11. arXiv:1406.6645Freely accessible. Bibcode:2014ApJ...791..121M. doi:10.1088/0004-637X/791/2/121. Retrieved 28 October 2017. 
  8. ^ a b c d e Tedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (October 2004). "IRAS Minor Planet Survey V6.0". NASA Planetary Data System. Bibcode:2004PDSS...12.....T. Archived from the original on 2016-06-03. Retrieved 28 October 2017. 
  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". The Astrophysical Journal Letters. 759 (1): 5. arXiv:1209.5794Freely accessible. Bibcode:2012ApJ...759L...8M. doi:10.1088/2041-8205/759/1/L8. Retrieved 28 October 2017. 
  10. ^ 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:1109.6407Freely accessible. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. Retrieved 28 October 2017. 
  11. ^ a b Behrend, Raoul. "Asteroids and comets rotation curves – (1275) Cimbria". Geneva Observatory. Retrieved 28 October 2017. 
  12. ^ a b Durech, J.; Hanus, J.; Oszkiewicz, D.; Vanco, R. (March 2016). "Asteroid models from the Lowell photometric database". Astronomy and Astrophysics. 587: 6. arXiv:1601.02909Freely accessible. Bibcode:2016A&A...587A..48D. doi:10.1051/0004-6361/201527573. Retrieved 28 October 2017. 
  13. ^ 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". The Astronomical Journal. 150 (3): 35. arXiv:1504.04041Freely accessible. Bibcode:2015AJ....150...75W. doi:10.1088/0004-6256/150/3/75. Retrieved 28 October 2017. 
  14. ^ a b 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:1506.00762Freely accessible. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. Retrieved 28 October 2017. 
  15. ^ a b "1275 Cimbria (1932 WG)". Minor Planet Center. Retrieved 28 October 2017. 
  16. ^ a b Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families" (PDF). Asteroids IV: 297–321. arXiv:1502.01628Freely accessible. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. Retrieved 28 October 2017. 

External links[edit]