1980 Tezcatlipoca

1980 Tezcatlipoca
Lightcurve-based 3D-model of Tezcatlipoca
Discovery [1]
Discovered by A. G. Wilson
A.A.E. Wallenquist
Discovery site Palomar Obs.
Discovery date 19 June 1950
Designations
MPC designation (1980) Tezcatlipoca
Named after
 Tezcatlipoca
(Aztec creator god)[2]
1950 LA
NEO · Amor [1][3]
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 66.96 yr (24,458 days)
Aphelion 2.3331 AU
Perihelion 1.0858 AU
1.7094 AU
Eccentricity 0.3648
2.24 yr (816 days)
328.60°
0° 26m 27.6s / day
Inclination 26.869°
246.57°
115.49°
Earth MOID 0.2455 AU · 95.6 LD
Physical characteristics
Dimensions 4.3 km (Gehrels)[1]
4.36±0.10[4]
4.50±0.04 km[5]
5.998 km[6]
6.00 km (taken)[7]
6.012±0.083 km[8]
6.66 km[9]
7.24612±0.00005 h[10]
7.2505±0.0008 h[11]
7.251±0.002 h[12]
7.25225 h[13]
7.25226±0.00005 h[14]
0.1279[6][7]
0.132±0.028[8]
0.145[9]
0.247±0.005[5]
0.25 (Gehrels)[1]
0.26±0.03[4]
0.47±0.43[15]
SU (Tholen)[1]
Sl (SMASS)[1]
Sw (ExploreNEOs)[16]
S (LCDB)[7]
B–V = 0.955[1]
U–B = 0.455[1]
13.6[9] · 13.87[4] · 13.92[1][5][8] · 13.96±0.1[6][7][11] · 14.30±1.07[17]

    1980 Tezcatlipoca, provisional designation 1950 LA, is an eccentric, stony asteroid and near-Earth object of the Amor group, approximately 6 kilometers in diameter.

    It was discovered on 19 June 1950, by American astronomer Albert Wilson and Swedish astronomer Åke Wallenquist at the U.S. Palomar Observatory in California.[3] It was named after the Aztech deity Tezcatlipoca.[2]

    Orbit and classification

    Tezcatlipoca orbits the Sun in the inner main-belt at a distance of 1.1–2.3 AU once every 2 years and 3 months (816 days). Its orbit has an eccentricity of 0.36 and an inclination of 27° with respect to the ecliptic.[1]

    This near-Earth object has an Earth minimum orbit intersection distance of 0.2455 AU (36,700,000 km), which corresponds to 95.6 lunar distances.[1] The body's observation arc begins with its official discovery observation at Palomar.[3]

    Physical characteristics

    The S-type asteroid is classified as a Sw-type by the ExploreNEOs project,[16] and as a SU and Sl-type on the Tholen and SMASS taxonomic scheme, respectively.[1]

    Between 1988 and 2015, five rotational lightcurves of Tezcatlipoca were obtained from photometric observations and gave a well-defined, concurring rotation period of 7.25 hours with a brightness variation between 0.22 and 1.01 in magnitude, indicative of a non-spheroidal shape (U=3/n.a./2+/3-/n.a.).[10][11][12][13][14]

    According to the surveys carried out by the Japanese Akari satellite and NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Tezcatlipoca measures between 4.36 and 6.012 kilometers in diameter and its surface has an albedo between 0.128 and 0.26.[4][5][6][8] The Collaborative Asteroid Lightcurve Link agrees with the revised NEOWISE observations, that is, an albedo of 0.128 and a diameter of 6.0 kilometers with an absolute magnitude of 13.96.[7]

    Naming

    This minor planet was named after Tezcatlipoca, the Aztec deity of matter, whose name translates to "Smoking Mirror" in the Nahuatl language. His animal counterpart was the jaguar and his contender was Quetzálcoatl, after which the minor planet 1915 Quetzálcoatl is named. Both deities are Aztec creator gods and were depicted as twin serpents that coil round each other to produce time.[2] The official naming citation was published by the Minor Planet Center before November 1977 (M.P.C. 4237).[18]

    References

    1. 1 2 3 4 5 6 7 8 9 10 11 12 13 "JPL Small-Body Database Browser: 1980 Tezcatlipoca (1950 LA)" (2017-06-05 last obs.). Jet Propulsion Laboratory. Retrieved 10 June 2017.
    2. 1 2 3 Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (1980) Tezcatlipoca. Springer Berlin Heidelberg. p. 160. ISBN 978-3-540-00238-3. Retrieved 30 August 2016.
    3. 1 2 3 "1980 Tezcatlipoca (1950 LA)". Minor Planet Center. Retrieved 30 August 2016.
    4. 1 2 3 4 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:1606.08923. Bibcode:2016AJ....152...63N. doi:10.3847/0004-6256/152/3/63. Retrieved 10 June 2017.
    5. 1 2 3 4 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 30 August 2016.
    6. 1 2 3 4 Pravec, Petr; Harris, Alan W.; Kusnirák, Peter; Galád, Adrián; Hornoch, Kamil (September 2012). "Absolute magnitudes of asteroids and a revision of asteroid albedo estimates from WISE thermal observations". Icarus. 221 (1): 365–387. Bibcode:2012Icar..221..365P. doi:10.1016/j.icarus.2012.07.026. Retrieved 30 August 2016.
    7. 1 2 3 4 5 "LCDB Data for (1980) Tezcatlipoca". Asteroid Lightcurve Database (LCDB). Retrieved 30 August 2016.
    8. 1 2 3 4 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:1109.6407. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. Retrieved 30 August 2016.
    9. 1 2 3 Harris, Alan W.; Davies, John K. (December 1999). "Physical Characteristics of Near-Earth Asteroids from Thermal Infrared Spectrophotometry". Icarus. 142 (2): 464–475. Bibcode:1999Icar..142..464H. doi:10.1006/icar.1999.6248. Retrieved 30 August 2016.
    10. 1 2 Behrend, Raoul. "Asteroids and comets rotation curves – (1980) Tezcatlipoca". Geneva Observatory. Retrieved 30 August 2016.
    11. 1 2 3 Wisniewski, W. Z.; Michalowski, T. M.; Harris, A. W.; McMillan, R. S. (March 1995). "Photoelectric Observations of 125 Asteroids". Abstracts of the Lunar and Planetary Science Conference. Bibcode:1995LPI....26.1511W. Retrieved 30 August 2016.
    12. 1 2 Warner, Brian D. (October 2015). "Near-Earth Asteroid Lightcurve Analysis at CS3-Palmer Divide Station: 2015 March–June". The Minor Planet Bulletin. 42 (4): 256–266. Bibcode:2015MPBu...42..256W. ISSN 1052-8091. Retrieved 30 August 2016.
    13. 1 2 Kaasalainen, Mikko; Pravec, Petr; Krugly, Yurij N.; Sarounová, Lenka; Torppa, Johanna; Virtanen, Jenni; et al. (January 2004). "Photometry and models of eight near-Earth asteroids". Icarus. 167 (1): 178–196. Bibcode:2004Icar..167..178K. doi:10.1016/j.icarus.2003.09.012. Retrieved 30 August 2016.
    14. 1 2 Hanus, J.; Delbo', M.; Durech, J.; Alí-Lagoa, V. (August 2015). "Thermophysical modeling of asteroids from WISE thermal infrared data – Significance of the shape model and the pole orientation uncertainties". Icarus. 256: 101–116. arXiv:1504.04199. Bibcode:2015Icar..256..101H. doi:10.1016/j.icarus.2015.04.014. Retrieved 30 August 2016.
    15. ↑ Thomas, C. A.; Trilling, D. E.; Emery, J. P.; Mueller, M.; Hora, J. L.; Benner, L. A. M.; et al. (September 2011). "ExploreNEOs. V. Average Albedo by Taxonomic Complex in the Near-Earth Asteroid Population". The Astronomical Journal. 142 (3): 12. Bibcode:2011AJ....142...85T. doi:10.1088/0004-6256/142/3/85. Retrieved 26 December 2015.
    16. 1 2 Thomas, Cristina A.; Emery, Joshua P.; Trilling, David E.; Delbó, Marco; Hora, Joseph L.; Mueller, Michael (January 2014). "Physical characterization of Warm Spitzer-observed near-Earth objects" (PDF). Icarus. 228: 217–246. arXiv:1310.2000. Bibcode:2014Icar..228..217T. doi:10.1016/j.icarus.2013.10.004. Retrieved 30 August 2016.
    17. ↑ 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 30 August 2016.
    18. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 30 August 2016.
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