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1801 Titicaca

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1801 Titicaca
Shape model of Titicaca from its lightcurve
Discovery[1]
Discovered byM. Itzigsohn
Discovery siteLa Plata Obs.
Discovery date23 September 1952
Designations
(1801) Titicaca
Named after
Lake Titicaca[2]
1952 SP1 · 1963 UR
main-belt · (outer)
Eos[3][4]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc64.61 yr (23,599 days)
Aphelion3.2256 AU
Perihelion2.8124 AU
3.0190 AU
Eccentricity0.0684
5.25 yr (1,916 days)
55.926°
0° 11m 16.44s / day
Inclination10.972°
77.603°
9.4673°
Physical characteristics
Dimensions19.31±0.41 km[5]
19.72±1.19 km[6]
21.957±0.296[7]
23.08 km (derived)[3]
23.18±2.4 km[8]
24.772±0.106 km[9]
3.2106±0.0005 h[10]
3.211233±0.000001 h[11]
0.1098 (derived)[3]
0.1146±0.0104[9]
0.1309±0.032[8]
0.172±0.018[5][7]
0.181±0.023[6]
S (assumed)[3]
11.0[6][8][9] · 11.10[5] · 11.2[1][3] · 11.32±0.22[12]

1801 Titicaca (prov. designation: 1952 SP1) is a stony Eos asteroid from the asteroid belt, approximately 22 kilometers in diameter. It was discovered on 23 September 1952, by Argentine astronomer Miguel Itzigsohn at La Plata Observatory in the capital of the province of Buenos Aires.[13] It was named after Lake Titicaca in South America.[2]

Orbit and classification

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Titicaca is a member of the Eos family (606), the largest asteroid family in the outer main belt consisting of nearly 10,000 asteroids.[4][14]: 23  It orbits the Sun at a distance of 2.8–3.2 AU once every 5 years and 3 months (1,916 days). Its orbit has an eccentricity of 0.07 and an inclination of 11° with respect to the ecliptic.[1] As no precoveries were taken, and no prior identifications were made, Titicaca's observation arc begins with its official discovery observation.[13]

Physical characteristics

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Titicaca is an assumed S-type asteroid.[3]

Rotation period

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In March 2007, a rotational lightcurve of Titicaca was obtained from photometric observations taken by German amateur astronomer Axel Martin. It gave a well-defined rotation period of 3.2106 hours with a brightness variation of 0.50 in magnitude (U=3).[10] A 2006-published lightcurve, constructed from photometry data from the Lowell photometric database, gave a concurring period of 3.211233 hours.[11]

Diameter and albedo

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According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Titicaca measures between 19.31 and 24.77 kilometers in diameter and its surface has an albedo between 0.11 and 0.18.[5][6][7][8][9] The Collaborative Asteroid Lightcurve Link derives an albedo of 0.109 and a diameter of 23.08 kilometers.[3]

Naming

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This minor planet was named after Lake Titicaca in the Andes, on the border of Peru and Bolivia at an altitude of 3,812 metres (12,507 feet) above sea level, the largest lake by volume in South America and one of the largest and highest lakes in the world.[2] Naming citation was published on 8 April 1982 (M.P.C. 6832).[15]

References

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  1. ^ a b c d "JPL Small-Body Database Browser: 1801 Titicaca (1952 SP1)" (2017-05-04 last obs.). Jet Propulsion Laboratory. Retrieved 3 June 2017.
  2. ^ a b c Schmadel, Lutz D. (2007). "(1801) Titicaca". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 144. doi:10.1007/978-3-540-29925-7_1802. ISBN 978-3-540-00238-3.
  3. ^ a b c d e f g "LCDB Data for (1801) Titicaca". Asteroid Lightcurve Database (LCDB). Retrieved 19 December 2016.
  4. ^ a b "Asteroid 1801 Titicaca – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 26 October 2019.
  5. ^ 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:1209.5794. Bibcode:2012ApJ...759L...8M. doi:10.1088/2041-8205/759/1/L8. Retrieved 19 December 2016.
  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. (online, AcuA catalog p. 153)
  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:1406.6645. Bibcode:2014ApJ...791..121M. doi:10.1088/0004-637X/791/2/121. Retrieved 19 December 2016.
  8. ^ a b c d Tedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (October 2004). "IRAS Minor Planet Survey V6.0". NASA Planetary Data System. 12: IRAS-A-FPA-3-RDR-IMPS-V6.0. Bibcode:2004PDSS...12.....T. Retrieved 22 October 2019.
  9. ^ 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". The Astrophysical Journal. 741 (2): 25. arXiv:1109.6407. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90.
  10. ^ a b Behrend, Raoul. "Asteroids and comets rotation curves – (1801) Titicaca". Geneva Observatory. Retrieved 19 December 2016.
  11. ^ 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:1601.02909. Bibcode:2016A&A...587A..48D. doi:10.1051/0004-6361/201527573. Retrieved 19 December 2016.
  12. ^ 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. Retrieved 19 December 2016.
  13. ^ a b "1801 Titicaca (1952 SP1)". Minor Planet Center. Retrieved 19 December 2016.
  14. ^ Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families". Asteroids IV. pp. 297–321. arXiv:1502.01628. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. ISBN 9780816532131.
  15. ^ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 19 December 2016.
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