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1333 Cevenola

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1333 Cevenola
Shape model of Cevenola from its lightcurve
Discovery[1]
Discovered byO. Bancilhon
Discovery siteAlgiers Obs.
Discovery date20 February 1934
Designations
(1333) Cevenola
PronunciationOccitan: [seveˈnɔlɔ]
Named after
Cévennes
(mountains, France)[2]
1934 DA · 1951 EX
main-belt · Eunomia[3]
Orbital characteristics[1]
Epoch 16 February 2017 (JD 2457800.5)
Uncertainty parameter 0
Observation arc82.31 yr (30,064 days)
Aphelion2.9864 AU
Perihelion2.2775 AU
2.6319 AU
Eccentricity0.1347
4.27 yr (1,560 days)
203.92°
0° 13m 50.88s / day
Inclination14.641°
115.10°
336.10°
Known satellites1
Physical characteristics
Dimensions11.2±1.4 km[4]
11.31±0.99 km[5]
14.54 km (calculated)[3]
15.24±0.74 km[6]
15.262±0.209 km[7]
17.146±0.237 km[8]
4.877±0.001 h[9]
4.8788±0.0004 h[10]
4.87932±0.00005 h[11]
4.880±0.003 h[10]
4.88±0.02 h[12]
4.88 h[4]
0.1662±0.0378[8]
0.209±0.030[6][7]
0.21 (assumed)[3]
0.214±0.081[4]
0.380±0.043[5]
Sq[13] · S[3]
11.4[5][6][8] · 11.5[1][3] · 12.05±0.12[4]

1333 Cevenola, provisional designation 1934 DA, is a binary Eunomian asteroid from the asteroid belt, approximately 15 kilometers in diameter. It was discovered on 20 February 1934, by French astronomer Odette Bancilhon at Algiers Observatory, Algeria in Northern Africa.[14] It was named after the French mountain-range Cévennes,[2] via the Occitan feminine adjective/demonym cevenòla (cévenole in French).

Description

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The S-type asteroid is a member of the Eunomia family.[3] More specifically, it is estimated to have a Sq spectral type, which would also agree with its family classification.[13] It orbits the Sun at a distance of 2.3–3.0 AU once every 4 years and 3 months (1,560 days). Its orbit has an eccentricity of 0.13 and an inclination of 15° with respect to the ecliptic.[1] As no precoveries were taken, and no prior identifications were made, the body's observation arc begins with its official discovery observation.[14]

Lightcurve-based 3D-model of Cevenola

Photometric lightcurve observations gave a well determined rotation period of 4.88 hours with a brightness variation between 0.57 and 1.1 magnitude (U=3/3/3/3/3).[4][9][10][11][12] The asteroid has a geometric albedo of 0.21, as measured by the Japanese Infrared Satellite, Akari, and by Spitzer's Infrared Spectrograph (IRS).[4][6] Observations by the NEO-/Wide-field Infrared Survey Explorer missions gave a somewhat different result of 0.17 and 0.38, respectively.[5][8] Determinations of the asteroid's diameter resulted in 11 kilometers for Spitzer and WISE/NEOWISE,[4][5] 15 kilometer for AKARAI and the LCDB's best calculations,[3][6] and 17 kilometers for the preliminary results of the NEOWISE mission.[8]

In October 2008, the discovery of a satellite in orbit of Cevenola was announced. The moon measures approximately 6 kilometers in diameter.[15][16]

The asteroid was named after the Cévennes, a mountain range in southern France at the eastern rim of the Massif Central.[2] Naming citation was first mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 121).[2]

S/2008 (1333) 1
Discovery
Discovery date12 October 2008 (announced)
Light curve
Orbital characteristics
Satellite of1333 Cevenola
Physical characteristics
Dimensions6.0±0.1 km
Volume113 km3 (assumed)

References

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  1. ^ a b c d "JPL Small-Body Database Browser: 1333 Cevenola (1934 DA)" (2016-06-13 last obs.). Jet Propulsion Laboratory. Retrieved 16 January 2017.
  2. ^ a b c d Schmadel, Lutz D. (2007). "(1333) Cevenola". Dictionary of Minor Planet Names – (1333) Cevenola. Springer Berlin Heidelberg. p. 109. doi:10.1007/978-3-540-29925-7_1334. ISBN 978-3-540-00238-3.
  3. ^ a b c d e f g "LCDB Data for (1333) Cevenola". Asteroid Lightcurve Database (LCDB). Retrieved 16 January 2017.
  4. ^ a b c d e f g 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. hdl:2060/20130014861. Retrieved 16 January 2017.
  5. ^ 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. Retrieved 16 January 2017.
  6. ^ a b c d e 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. (online, AcuA catalog p. 153)
  7. ^ a b 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:1406.6645. Bibcode:2014ApJ...791..121M. doi:10.1088/0004-637X/791/2/121. Retrieved 16 January 2017.
  8. ^ a b c d e Mainzer, A.; Grav, T.; Masiero, J.; Hand, E.; Bauer, J.; Tholen, D.; et al. (November 2011). "NEOWISE Studies of Spectrophotometrically Classified Asteroids: Preliminary Results". The Astrophysical Journal. 741 (2): 25. arXiv:1109.6407. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90.
  9. ^ a b Warner, Brian D. (April 2011). "Upon Further Review: VI. An Examination of Previous Lightcurve Analysis from the Palmer Divide Observatory". The Minor Planet Bulletin. 38 (2): 96–101. Bibcode:2011MPBu...38...96W. ISSN 1052-8091. Retrieved 16 January 2017.
  10. ^ a b c Behrend, Raoul. "Asteroids and comets rotation curves – (1333) Cevenola". Geneva Observatory. Retrieved 16 January 2017.
  11. ^ a b Hanus, J.; Durech, J.; Broz, M.; Warner, B. D.; Pilcher, F.; Stephens, R.; et al. (June 2011). "A study of asteroid pole-latitude distribution based on an extended set of shape models derived by the lightcurve inversion method". Astronomy & Astrophysics. 530: 16. arXiv:1104.4114. Bibcode:2011A&A...530A.134H. doi:10.1051/0004-6361/201116738. Retrieved 16 January 2017.
  12. ^ a b Warner, B. D. (December 2002). "Asteroid Photometry at the Palmer Divide Observatory: Results for 1333 Cevenola and 2460 Mitlincoln". The Minor Planet Bulletin. 29: 74–75. Bibcode:2002MPBu...29...74W. Retrieved 16 January 2017.
  13. ^ a b Birlan, M.; Nedelcu, D. A.; Descamps, P.; Berthier, J.; Marchis, F.; Merouane, S.; et al. (July 2011). "Spectral properties of (854) Frostia, (1333) Cevenola and (3623) Chaplin". Monthly Notices of the Royal Astronomical Society. 415 (1): 587–595. Bibcode:2011MNRAS.415..587B. doi:10.1111/j.1365-2966.2011.18740.x.
  14. ^ a b "1333 Cevenola (1934 DA)". Minor Planet Center. Retrieved 16 January 2017.
  15. ^ Johnston, Robert. "(1333) Cevenola". johnstonsarchive.net. Retrieved 28 May 2015.
  16. ^ Birlan, Mirel; Nedelcu, D.; Descamps, P.; Berthier, J.; Marchis, F.; Merouane, S. (September 2008). "Spectral Investigation of Binary Asteroids". American Astronomical Society. 40: 28.20. Bibcode:2008DPS....40.2820B. Retrieved 3 November 2015.
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