Astronomy:1801 Titicaca

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1801 Titicaca
001801-asteroid shape model (1801) Titicaca.png
Shape model of Titicaca from its lightcurve
Discovery[1]
Discovered byM. Itzigsohn
Discovery siteLa Plata Obs.
Discovery date23 September 1952
Designations
(1801) Titicaca
Named afterLake Titicaca[2]
1952 SP1 · 1963 UR
Minor planet categorymain-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)
|{{{apsis}}}|helion}}3.2256 AU
|{{{apsis}}}|helion}}2.8124 AU
3.0190 AU
Eccentricity0.0684
Orbital period5.25 yr (1,916 days)
Mean anomaly55.926°
Mean motion0° 11m 16.44s / day
Inclination10.972°
Longitude of ascending node77.603°
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]
Rotation period3.2106±0.0005 h[10]
3.211233±0.000001 h[11]
Geometric albedo0.1098 (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]
Absolute magnitude (H)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

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

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

Rotation period

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 ({{{1}}}).[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

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

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

  1. ↑ 1.0 1.1 1.2 1.3 "JPL Small-Body Database Browser: 1801 Titicaca (1952 SP1)". Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2001801. Retrieved 3 June 2017. 
  2. ↑ 2.0 2.1 2.2 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. ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 "LCDB Data for (1801) Titicaca". Asteroid Lightcurve Database (LCDB). http://www.minorplanet.info/PHP/generateOneAsteroidInfo.php?AstInfo=1801%7CTiticaca. Retrieved 19 December 2016. 
  4. ↑ 4.0 4.1 "Asteroid 1801 Titicaca – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. https://sbntools.psi.edu/ferret/SimpleSearch/results.action?targetName=1801+Titicaca#Asteroid%201801%20TiticacaEAR-A-VARGBDET-5-NESVORNYFAM-V3.0. Retrieved 26 October 2019. 
  5. ↑ 5.0 5.1 5.2 5.3 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. doi:10.1088/2041-8205/759/1/L8. Bibcode: 2012ApJ...759L...8M. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2012ApJ...759L...8M. Retrieved 19 December 2016. 
  6. ↑ 6.0 6.1 6.2 6.3 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. doi:10.1093/pasj/63.5.1117. Bibcode: 2011PASJ...63.1117U.  (online, AcuA catalog p. 153)
  7. ↑ 7.0 7.1 7.2 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. doi:10.1088/0004-637X/791/2/121. Bibcode: 2014ApJ...791..121M. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2014ApJ...791..121M. Retrieved 19 December 2016. 
  8. ↑ 8.0 8.1 8.2 8.3 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. https://sbnarchive.psi.edu/pds3/iras/IRAS_A_FPA_3_RDR_IMPS_V6_0/data/diamalb.tab. Retrieved 22 October 2019. 
  9. ↑ 9.0 9.1 9.2 9.3 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. doi:10.1088/0004-637X/741/2/90. Bibcode: 2011ApJ...741...90M. 
  10. ↑ 10.0 10.1 Behrend, Raoul. "Asteroids and comets rotation curves – (1801) Titicaca". Geneva Observatory. http://obswww.unige.ch/~behrend/page4cou.html#001801. Retrieved 19 December 2016. 
  11. ↑ 11.0 11.1 Durech, J.; Hanus, J.; Oszkiewicz, D.; Vanco, R. (March 2016). "Asteroid models from the Lowell photometric database". Astronomy and Astrophysics 587: 6. doi:10.1051/0004-6361/201527573. Bibcode: 2016A&A...587A..48D. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2016A&A...587A..48D. 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. doi:10.1016/j.icarus.2015.08.007. Bibcode: 2015Icar..261...34V. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2015Icar..261...34V. Retrieved 19 December 2016. 
  13. ↑ 13.0 13.1 "1801 Titicaca (1952 SP1)". Minor Planet Center. https://www.minorplanetcenter.net/db_search/show_object?object_id=1801. 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. doi:10.2458/azu_uapress_9780816532131-ch016. ISBN 9780816532131. Bibcode: 2015aste.book..297N. 
  15. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. https://www.minorplanetcenter.net/iau/ECS/MPCArchive/MPCArchive_TBL.html. Retrieved 19 December 2016. 

External links



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