Astronomy:512 Taurinensis

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Short description: Mars-crossing asteroid
512 Taurinensis
512Taurinensis (Lightcurve Inversion).png
Lightcurve-based 3D-model of Taurinensis
Discovery [1]
Discovered byM. F. Wolf
Discovery siteHeidelberg Obs.
Discovery date23 June 1903
Designations
(512) Taurinensis
Pronunciation/tɔːrɪˈnɛnsɪs/
Named afterTurin [2] (Italian city)
1903 LV · A909 GE
Minor planet categoryMars-crosser [1][3][4]
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc108.23 yr (39,532 days)
|{{{apsis}}}|helion}}2.7466 AU
|{{{apsis}}}|helion}}1.6323 AU
2.1895 AU
Eccentricity0.2545
Orbital period3.24 yr (1,183 days)
Mean anomaly30.908°
Mean motion0° 18m 15.12s / day
Inclination8.7463°
Longitude of ascending node107.04°
249.36°
Earth MOID0.6518 AU · 253.9 LD
Mars MOID0.2980 AU
Physical characteristics
Dimensions18.70±1.87 km[5]
20.87±0.36 km[6]
23.09±1.4 km[7]
Rotation period5.5804±0.0006 h[8]
5.582 h[9]
5.583±0.001 h[10]
5.585±0.001 h[11]
5.59 h[12]
Geometric albedo0.1772±0.024[7]
0.225±0.010[6]
0.270±0.054[5]
Tholen = S [1]
SMASS = S [1][4]
B–V = 0.917 [1]
U–B = 0.525 [1]
Absolute magnitude (H)10.68[1][5][6][7] · 10.72[4] · 10.72±0.04[11][13] · 10.72±0.40[14]


Taurinensis (minor planet designation: 512 Taurinensis), provisional designation 1903 LV, is a stony asteroid and large Mars-crosser on an eccentric orbit from the inner regions of the asteroid belt, approximately 20 kilometers in diameter. It was discovered on 23 June 1903, by astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory in southwest Germany.[3] The asteroid was named after the Italian city of Turin.[2] It is the 4th-largest Mars-crossing asteroid.

Orbit and classification

Taurinensis is a Mars-crossing asteroid, a dynamically unstable group between the main belt and the near-Earth populations, crossing the orbit of Mars at 1.666 AU. It orbits the Sun at a distance of 1.6–2.7 AU once every 3 years and 3 months (1,183 days). Its orbit has an eccentricity of 0.25 and an inclination of 9° with respect to the ecliptic.[1] The body's observation arc begins with its identification as A909 GE at Heidelberg in April 1909, almost 6 years prior to its official discovery observation.[3]

Physical characteristics

Taurinensis is a common, stony S-type asteroid in both the Tholen and SMASS classification.[1]

Rotation period

In 1982, the asteroid was observed using photometry from the La Silla Observatory to generate a composite light curve. The resulting data showed a rotation period of 0.2326 days (5.58 h) with a brightness variation of 0.2 in magnitude.[4][9]

Diameter and albedo

According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Taurinensis measures between 18.70 and 23.09 kilometers in diameter and its surface has an albedo between 0.1772 and 0.270.[5][6][7] The Collaborative Asteroid Lightcurve Link adopts the results obtained by IRAS, that is, an albedo of 0.1772 and a diameter of 23.09 kilometers based on an absolute magnitude of 10.72.[4]

With a mean-diameter of 20 kilometers, Taurinensis is the 4th-largest Mars-crossing asteroids, just behind 132 Aethra (43 km), 323 Brucia (36 km) and 2204 Lyyli (25 km), and larger than 1508 Kemi (17 km), 1474 Beira (15 km) and 1310 Villigera (14 km).

Naming

This minor planet was named after "Taurinensis", the Latin name of the city of Turin, located in northern Italy. It was named in 1905, by astronomers of the Observatory of Turin with the discoverer's endorsement (AN 167, 239). The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 55).[2]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 "JPL Small-Body Database Browser: 512 Taurinensis (1903 LV)". Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2000512. 
  2. ↑ 2.0 2.1 2.2 Schmadel, Lutz D. (2007). "(512) Taurinensis". Dictionary of Minor Planet Names – (512) Taurinensis. Springer Berlin Heidelberg. p. 55. doi:10.1007/978-3-540-29925-7_513. ISBN 978-3-540-00238-3. 
  3. ↑ 3.0 3.1 3.2 "512 Taurinensis (1903 LV)". Minor Planet Center. https://www.minorplanetcenter.net/db_search/show_object?object_id=512. 
  4. ↑ 4.0 4.1 4.2 4.3 4.4 "LCDB Data for (512) Taurinensis". Asteroid Lightcurve Database (LCDB). http://www.minorplanet.info/PHP/generateOneAsteroidInfo.php?AstInfo=512%7CTaurinensis. 
  5. ↑ 5.0 5.1 5.2 5.3 Alí-Lagoa, V.; Delbo', M. (July 2017). "Sizes and albedos of Mars-crossing asteroids from WISE/NEOWISE data". Astronomy and Astrophysics 603: 8. doi:10.1051/0004-6361/201629917. Bibcode: 2017A&A...603A..55A. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2017A&A...603A..55A. Retrieved 26 October 2017. 
  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 7.3 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. 
  8. ↑ Benishek, Vladimir (October 2016). "Lightcurves and Rotation Periods for 14 Asteroids". The Minor Planet Bulletin 43 (4): 339–342. ISSN 1052-8091. Bibcode: 2016MPBu...43..339B. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2016MPBu...43..339B. Retrieved 26 October 2017. 
  9. ↑ 9.0 9.1 Lagerkvist, C.-I.; Kamel, L. (December 1982). "Physical studies of asteroids. X - Photoelectric light curves of the asteroids 219 and 512". Moon and the Planets 27 (4): 463–466. doi:10.1007/BF00929999. Bibcode: 1982M&P....27..463L. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=1982M&P....27..463L. Retrieved 26 October 2017. 
  10. ↑ Behrend, Raoul. "Asteroids and comets rotation curves – (512) Taurinensis". Geneva Observatory. http://obswww.unige.ch/~behrend/page2cou.html#000512. 
  11. ↑ 11.0 11.1 Harris, A. W.; Young, J. W.; Dockweiler, Thor; Gibson, J.; Poutanen, M.; Bowell, E. (January 1992). "Asteroid lightcurve observations from 1981". Icarus 95 (1): 115–147.ResearchsupportedbyLowellObservatoryEndowmentandNASA. doi:10.1016/0019-1035(92)90195-D. ISSN 0019-1035. Bibcode: 1992Icar...95..115H. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=1992Icar...95..115H. Retrieved 26 October 2017. 
  12. ↑ Piironen, J.; Lagerkvist, C.-I.; Erikson, A.; Oja, T.; Magnusson, P.; Festin, L. et al. (March 1998). "Physical studies of asteroids. XXXII. Rotation periods and UBVRI-colours for selected asteroids". Astronomy and Astrophysics Supplement 128 (3): 525–540. doi:10.1051/aas:1998393. Bibcode: 1998A&AS..128..525P. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=1998A&AS..128..525P. Retrieved 26 October 2017. 
  13. ↑ 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. doi:10.1016/j.icarus.2012.07.026. Bibcode: 2012Icar..221..365P. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2012Icar..221..365P. Retrieved 26 October 2017. 
  14. ↑ 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 26 October 2017. 

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