814 Tauris

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814 Tauris
Discovery  [1]
Discovered by G. Neujmin
Discovery site Simeiz Obs.
Discovery date2 January 1916
Designations
(814) Tauris
Pronunciation ⫽ˈtɔːrɪs⫽
Named after
 Crimea, (peninsula on the Black Sea in Eastern Europe) [2]
A916 AE ·1927 BA
A907 JE ·1916 YT
Orbital characteristics   [3]
Epoch 31 May 2020 (JD 2459000.5)
Uncertainty parameter 0
Observation arc 104.01 yr (37,990 d)
Aphelion 4.1233 AU
Perihelion 2.1884 AU
3.1558 AU
Eccentricity 0.3065
5.61 yr (2,048 d)
247.26°
0° 10m 32.88s / day
Inclination 21.822°
88.786°
296.53°
TJupiter 3.0250
Physical characteristics
Dimensions109.0  km × 109.0  km
Mass (9.74 ± 5.16/3.17)×1017 kg [7]
Mean density
1.74 ± 0.923/0.566 g/cm3 [7]
35.8  h [10] [11] [12]
36.081±30% h [3]

    814 Tauris ( prov. designation:A916 AEor1916 YT) is a dark and very large background asteroid, approximately 109 kilometers (68 miles) in diameter, located the outer regions of the asteroid belt. It was discovered on 2 January 1916, by astronomer Russian Grigory Neujmin at the Simeiz Observatory on Crimea. [1] The carbonaceous C-type asteroid has a longer-than average rotation period of 35.8 hours. It was named after the ancient name of the Crimean peninsula where the discovering observatory is located. [2]

    Contents

    Orbit and classification

    Tauris is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. [4] [5] It orbits the Sun in the outer main-belt at a distance of 2.2–4.1  AU once every 5 years and 7 months (2,048 days; semi-major axis of 3.16 AU). Its orbit has a notably high eccentricity of 0.31 and an inclination of 22° with respect to the ecliptic. [3] This gives it a TJupiter of 3.0250, near the boundary of 3, which separates asteroids (above 3) from the Jupiter-family comets (below 3). [3] Tauris was first observed as A907 JE at Taunton Observatory ( 803 ) on 12 May 1907. The body's observation arc begins at Heidelberg Observatory on 30 January 1916, or four weeks after its official discovery observation at Simeiz Observatory. [1]

    Naming

    This minor planet was named after the ancient name of the Crimean peninsula, Tauris. Lutz Schmadel, the author of the Dictionary of Minor Planet Names also mentions a mountain with the same name on the southwest coast of Crimea. In addition, Baltic German astronomer Ludwig von Struve (1858–1920) also taught astronomy at the Tavrida University (Tauris University) in Simferopol, a large city on the Crimean peninsula (R. Bremer). The naming was also mentioned in The Names of the Minor Planets by Paul Herget in 1955 ( H 81 ). [2]

    Physical characteristics

    In the Tholen classification as well in the Bus–Binzel SMASS classification, Tauris is a common, carbonaceous C-type asteroid, [3] while in both the Tholen- and SMASS-like taxonomy of the Small Solar System Objects Spectroscopic Survey (S3OS2), it is an X-type asteroid. [5] [13]

    Rotation period

    In 1983, a rotational lightcurve of Tauris, obtained from photometric observations with the ESO 0.5-metre telescope at La Silla, Chile, was by published by Belgian astronomer Henri Debehogne in collaboration with Italian astronomers Giovanni de Sanctis and Vincenzo Zappalà. Lightcurve analysis gave a rotation period of 35.8 hours with a brightness variation of 0.20 magnitude ( U=2 ). [10] In May 2013, Michael S. Alkema at the Elephant Head Observatory ( G35 ) in Arizona determined an identical period of 35.8±0.1 hours with an amplitude of 0.18±0.03 magnitude ( U=2– ). [11]

    Diameter and albedo

    According to the surveys carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, the Infrared Astronomical Satellite IRAS, and the Japanese Akari satellite, Tauris measures (102.229±2.138), (109.56±3.1) and (109.76±2.78) kilometers in diameter and its surface has an albedo of (0.054±0.011), (0.0470±0.003) and (0.047±0.003), respectively. [6] [8] [9] The Collaborative Asteroid Lightcurve Link adopts the results obtained by IRAS, that is, an albedo of 0.0470 and a diameter of 109.56 kilometers based on an absolute magnitude of 8.74. [12] Alternative mean-diameter measurements published by the WISE team include (98.77±33.90  km ), (104.357±28.04 km), (109.854±1.947 km) and (121.55±44.26 km) with corresponding albedos of (0.05±0.05), (0.0445±0.0344), (0.0444±0.0066) and (0.036±0.015). [5] [12]

    Several asteroid occultations of Tauris were observed between 1999 and 2015. [5] These timed observations are taken when the asteroid passes in front of a distant star. The two best-rated observations made on 26 and 29 July 2015, gave a best-fit ellipse dimension of (109.0 km × 109.0 km) and (110.0 km × 110.0 km), respectively. However, these two observations still received a relatively poor quality rating. [5]

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    References

    1. 1 2 3 4 5 "814 Tauris (A916 AE)". Minor Planet Center. Retrieved 25 March 2020.
    2. 1 2 3 Schmadel, Lutz D. (2007). "(814) Tauris". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 75. doi:10.1007/978-3-540-29925-7_815. ISBN   978-3-540-00238-3.
    3. 1 2 3 4 5 6 7 8 9 10 11 12 13 "JPL Small-Body Database Browser: 814 Tauris (A916 AE)" (2020-02-03 last obs.). Jet Propulsion Laboratory . Retrieved 25 March 2020.
    4. 1 2 "Asteroid 814 Tauris – Proper Elements". AstDyS-2, Asteroids – Dynamic Site. Retrieved 25 March 2020.
    5. 1 2 3 4 5 6 "Asteroid 814 Tauris – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 25 March 2020.
    6. 1 2 3 4 Mainzer, A. K.; Bauer, J. M.; Cutri, R. M.; Grav, T.; Kramer, E. A.; Masiero, J. R.; et al. (June 2016). "NEOWISE Diameters and Albedos V1.0". NASA Planetary Data System. Bibcode:2016PDSS..247.....M . Retrieved 25 March 2020.
    7. 1 2 3 Fienga, A.; Avdellidou, C.; Hanuš, J. (February 2020). "Asteroid masses obtained with INPOP planetary ephemerides". Monthly Notices of the Royal Astronomical Society. 492 (1). doi: 10.1093/mnras/stz3407 .
    8. 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 25 March 2020.
    9. 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)
    10. 1 2 Debehogne, H.; de Sanctis, G.; Zappala, V. (August 1983). "Photoelectric photometry of asteroids 45, 120, 776, 804, 814, and 1982DV". Icarus. 55 (2): 236–244. Bibcode:1983Icar...55..236D. doi:10.1016/0019-1035(83)90078-7. ISSN   0019-1035.
    11. 1 2 Alkema, Michael S. (October 2013). "Asteroid Lightcurve Analysis at Elephant Head Observatory: 2013 April-July" (PDF). Minor Planet Bulletin. 40 (4): 215–216. Bibcode:2013MPBu...40..215A. ISSN   1052-8091. Archived from the original (PDF) on 24 February 2020. Retrieved 25 March 2020.
    12. 1 2 3 4 "LCDB Data for (814) Tauris". Asteroid Lightcurve Database (LCDB). Retrieved 25 March 2020.
    13. 1 2 Lazzaro, D.; Angeli, C. A.; Carvano, J. M.; Mothé-Diniz, T.; Duffard, R.; Florczak, M. (November 2004). "S3OS2: the visible spectroscopic survey of 820 asteroids" (PDF). Icarus. 172 (1): 179–220. Bibcode:2004Icar..172..179L. doi:10.1016/j.icarus.2004.06.006 . Retrieved 25 March 2020.
    14. ↑ Warner, Brian D. (December 2007). "Initial Results of a Dedicated H-G Project" (PDF). Minor Planet Bulletin. 34 (4): 113–119. Bibcode:2007MPBu...34..113W. ISSN   1052-8091. Archived from the original (PDF) on 20 February 2020. Retrieved 25 March 2020.
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