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2013 Tucapel

From Wikipedia, the free encyclopedia
Main-belt asteroid

2013 Tucapel
Discovery[1]
Discovered byUniversity of Chile
(National Astronomical Observatory of Chile)
Discovery siteCerro El Roble Stn.
Discovery date22 October 1971
Designations
(2013) Tucapel
Named after
Battle of Tucapel[2]
1971 UH4 · 1936 PL
1940 XC · 1942 EP1
1950 TP2 · 1969 AT
1974 MM · 1974 NA
1974 OJ
main-belt · Flora[3]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc76.32 yr (27,876 days)
Aphelion2.8074AU
Perihelion1.7714 AU
2.2894 AU
Eccentricity0.2263
3.46yr (1,265 days)
130.64°
0° 17m 4.2s / day
Inclination7.5036°
96.545°
238.12°
Physical characteristics
Dimensions10.61±0.72 km[4]
11.187±0.380 km[5]
11.84 km(calculated)[3]
12.16±0.75 km[6]
12.685±0.065 km[7]
9.028±0.008h[8]
0.1003±0.0179[7]
0.110±0.014[6]
0.24(assumed)[3]
0.328±0.044[4][5]
S[3]
11.70[4] · 11.8[1][3] · 12.27±0.61[9] · 12.6[6][7]

2013 Tucapel, provisional designation1971 UH4, is an eccentric Florianasteroid from the inner regions of theasteroid belt, approximately 11 kilometers in diameter. It was discovered on 22 October 1971, by the University of Chile'sNational Astronomical Observatory atCerro El Roble Astronomical Station.[10] It was named for one of the indigenous Mapuche chiefs.

Orbit and classification

[edit]

Tucapel is a member of theFlora family, one of the largest groups of stony asteroids. It orbits the Sun in theinner main-belt at a distance of 1.8–2.8 AU once every 3 years and 6 months (1,265 days). Its orbit has aneccentricity of 0.23 and aninclination of 8° with respect to theecliptic.[1]

It was first observed as1936 PL atJohannesburg Observatory in 1936. Its first used observation was taken atTurku Observatory in 1942, when it was identified as1942 EP1, thereby extending the body'sobservation arc by 29 years prior to its official discovery observation at Cerro El Roble.[10]

Physical characteristics

[edit]

Tucapel has been characterized as a commonS-type asteroid.[3]

Rotation period

[edit]

In October 2009, a rotationallightcurve ofTucapel was obtained from photometric observations at the Oakley Southern Sky Observatory (E09) in Australia. Lightcurve analysis gave a well-definedrotation period of 9.028 hours with a brightness variation of 0.34magnitude (U=3).[8]

Diameter and albedo

[edit]

According to the surveys carried out by the JapaneseAkari satellite and NASA'sWide-field Infrared Survey Explorer with its subsequentNEOWISE mission,Tucapel measures between 10.61 and 12.685 kilometers in diameter and its surface has analbedo between 0.1003 and 0.328.[4][5][6][7] TheCollaborative Asteroid Lightcurve Link assumes an albedo of 0.24 — derived from8 Flora, the family's largest member and namesake – and calculates a diameter of 11.84 kilometers with anabsolute magnitude of 11.8.[3]

Naming

[edit]

Thisminor planet was named for one of the brave chiefs of theMapuche, indigenous inhabitants of south-central Chile and southwestern Argentina, who, with his wife Gualeva, victoriously entered the city of Imperial. He died in 1560, fighting against the colonial Spaniards(also seeArauco War,Battle of Tucapel andLautaro).[2] The official naming citation was published by theMinor Planet Center on 1 June 1980 (M.P.C. 5359).[11]

References

[edit]
  1. ^abcd"JPL Small-Body Database Browser: 2013 Tucapel (1971 UH4)" (2017-03-29 last obs.).Jet Propulsion Laboratory. Retrieved10 June 2017.
  2. ^abSchmadel, Lutz D. (2007). "(2013) Tucapel".Dictionary of Minor Planet Names – (2013) Tucapel.Springer Berlin Heidelberg. p. 163.doi:10.1007/978-3-540-29925-7_2014.ISBN 978-3-540-00238-3.
  3. ^abcdefg"LCDB Data for (2013) Tucapel". Asteroid Lightcurve Database (LCDB). Retrieved8 December 2016.
  4. ^abcdMasiero, 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. Retrieved8 December 2016.
  5. ^abcMasiero, 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. Retrieved8 December 2016.
  6. ^abcdUsui, 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. ^abcdMainzer, 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.
  8. ^abKrotz, Jonathan; Albers, Kendra; Carbo, Landry; Kragh, Katherine; Meiers, Andrew; Yim, Arnold; et al. (July 2010)."Asteroid Lightcurve Analysis at the Oakley Southern Sky Observatory".The Minor Planet Bulletin.37 (3):99–101.Bibcode:2010MPBu...37...99K.ISSN 1052-8091. Retrieved8 December 2016.
  9. ^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. Retrieved8 December 2016.
  10. ^ab"2013 Tucapel (1971 UH4)".Minor Planet Center. Retrieved8 December 2016.
  11. ^"MPC/MPO/MPS Archive".Minor Planet Center. Retrieved8 December 2016.


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