512 Taurinensis
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 after
Turin [2] (Italian city)
1903 LV · A909 GE
Mars-crosser [1][3][4]
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc108.23 yr (39,532 days)
Aphelion2.7466 AU
Perihelion1.6323 AU
2.1895 AU
Eccentricity0.2545
3.24 yr (1,183 days)
30.908°
0° 18m 15.12s / day
Inclination8.7463°
107.04°
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]
5.5804±0.0006 h[8]
5.582 h[9]
5.583±0.001 h[10]
5.585±0.001 h[11]
5.59 h[12]
0.1772±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]
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 2 3 4 5 6 7 8 9 10 "JPL Small-Body Database Browser: 512 Taurinensis (1903 LV)" (2017-07-05 last obs.). Jet Propulsion Laboratory. Retrieved 26 October 2017.
    2. 1 2 3 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. 1 2 3 "512 Taurinensis (1903 LV)". Minor Planet Center. Retrieved 26 October 2017.
    4. 1 2 3 4 5 "LCDB Data for (512) Taurinensis". Asteroid Lightcurve Database (LCDB). Retrieved 26 October 2017.
    5. 1 2 3 4 Alí-Lagoa, V.; Delbo', M. (July 2017). "Sizes and albedos of Mars-crossing asteroids from WISE/NEOWISE data". Astronomy and Astrophysics. 603: 8. arXiv:1705.10263. Bibcode:2017A&A...603A..55A. doi:10.1051/0004-6361/201629917. Retrieved 26 October 2017.
    6. 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. (online, AcuA catalog p. 153)
    7. 1 2 3 4 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.
    8. ↑ Benishek, Vladimir (October 2016). "Lightcurves and Rotation Periods for 14 Asteroids". The Minor Planet Bulletin. 43 (4): 339–342. Bibcode:2016MPBu...43..339B. ISSN 1052-8091. Retrieved 26 October 2017.
    9. 1 2 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. Bibcode:1982M&P....27..463L. doi:10.1007/BF00929999. Retrieved 26 October 2017.
    10. ↑ Behrend, Raoul. "Asteroids and comets rotation curves – (512) Taurinensis". Geneva Observatory. Retrieved 26 October 2017.
    11. 1 2 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. Bibcode:1992Icar...95..115H. doi:10.1016/0019-1035(92)90195-D. ISSN 0019-1035. 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. Bibcode:1998A&AS..128..525P. doi:10.1051/aas:1998393. 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. Bibcode:2012Icar..221..365P. doi:10.1016/j.icarus.2012.07.026. 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. arXiv:1506.00762. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. Retrieved 26 October 2017.
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