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Revision as of 20:20, 8 August 2019

17 Thetis
Star field showing asteroid Thetis in the center
Discovery [1]
Discovered byR. Luther
Discovery siteDüsseldorf-Bilk Obs.
Discovery date17 April 1852
Designations
(17) Thetis
Pronunciation/ˈθiːtɪs/ (THEE-tis)
Named after
Thetis (Greek mythology)[2]
1954 SO1 · A913 CA
A916 YF
main-belt [3] · (inner)
AdjectivesThetidian
Symbol
Orbital characteristics [1]
Epoch 16 February 2017 (JD 2457800.5)
Uncertainty parameter 0
Observation arc164.55 yr (60,102 days)
Aphelion2.7987 AU
Perihelion2.1436 AU
2.4712 AU
Eccentricity0.1325
3.88 yr (1,419 days)
18.87 km/s
100.44°
0° 15m 13.32s / day
Inclination5.5902°
125.56°
136.10°
Physical characteristics
Dimensions84.899±2.027[4]
90±3.7km (IRAS)[5]
93.335±2.627[6]
Mass1.2×1018 kg[7][a]
Mean density
3.21±0.92 g/cm³[7]
12.27048±0.00001[8][9]
0.193±0.028[4]
B–V = 0.829[1]
U–B = 0.438[1]
S (Tholen)[1]
Sl (SMASS)[1] · S [8]
7.76[1][5][6] · 7.85[9]

Thetis (THEE-tis; minor planet designation: 17 Thetis) and provisional designation A913 CA, is a stony asteroid from the inner regions of the asteroid belt, approximately 90 kilometers in diameter. It was discovered on 17 April 1852, by German astronomer Robert Luther at Bilk Observatory in Düsseldorf, Germany.[3] He named his first asteroid discovery after Thetis from Greek mythology.[2]

Description

The asteroid orbits the Sun at a distance of 2.1–2.8 AU once every 3 years and 11 months (1,419 days). Its orbit has an eccentricity of 0.13 and an inclination of 6° with respect to the ecliptic.[1]

The spectrum of this object indicates that it is an S-type asteroid with both low and high calcium forms of pyroxene on the surface, along with less than 20% olivine. The high-calcium form of pyroxene forms 40% or more of the total pyroxene present, indicating a history of igneous rock deposits. This suggests that the asteroid underwent differentiation by melting, creating a surface of basalt rock.[10]

The mass of Thetis has been calculated from perturbations by 4 Vesta and 11 Parthenope. In 2007, Baer and Chesley calculated Thetis to have a mass of 1.2×1018 kg[a] with a density of 3.21 g/cm³.[7]

One Thetidian stellar occultation was observed from Oregon in 1999. However, the event was not timed.

This minor planet was named after Thetis, the mother of Achilles in Greek mythology.[2]

Notes

  1. ^ a b Thetismass2007: Mass of Thetis 0.00617 / Mass of Ceres 4.75) * Mass of Ceres 9.43E+20 = 1.224E+18, based on Baer 2008[7]

References

  1. ^ a b c d e f g h "JPL Small-Body Database Browser: 17 Thetis" (2016-11-11 last obs.). Jet Propulsion Laboratory. Retrieved 24 March 2017.
  2. ^ a b c Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (17) Thetis. Springer Berlin Heidelberg. p. 17. doi:10.1007/978-3-540-29925-7_18. ISBN 978-3-540-00238-3.
  3. ^ a b "17 Thetis". Minor Planet Center. Retrieved 24 March 2017.
  4. ^ a b 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. arXiv:1406.6645. Bibcode:2014ApJ...791..121M. doi:10.1088/0004-637X/791/2/121.
  5. ^ a b Tedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (October 2004). "IRAS Minor Planet Survey V6.0". NASA Planetary Data System: IRAS-A-FPA-3-RDR-IMPS-V6.0. Bibcode:2004PDSS...12.....T.
  6. ^ a b 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. arXiv:1109.6407. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90.
  7. ^ a b c d Baer, James; Chesley, Steven R. (January 2008). "Astrometric masses of 21 asteroids, and an integrated asteroid ephemeris". Celestial Mechanics and Dynamical Astronomy. 100 (1): 27–42. Bibcode:2008CeMDA.100...27B. doi:10.1007/s10569-007-9103-8.
  8. ^ a b "LCDB Data for (17) Thetis". Asteroid Lightcurve Database (LCDB). Retrieved 24 March 2017.
  9. ^ a b Michalowski, T.; Velichko, F. P.; Di Martino, M.; Krugly, Yu. N.; Kalashnikov, V. G.; Shevchenko, V. G.; et al. (December 1995). "Models of four asteroids: 17 Thetis, 52 Europa, 532 Herculina, and 704 Interamnia". Icarus. 118 (2): 292–301. Bibcode:1995Icar..118..292M. doi:10.1006/icar.1995.1192.
  10. ^ Sunshine, Jessica M.; Bus, Schelte J.; McCoy, Timothy J.; Burbine, Thomas H.; Corrigan, Catherine M.; Binzel, Richard P. (August 2004). "High-calcium pyroxene as an indicator of igneous differentiation in asteroids and meteorites". Meteoritics and Planetary Science. 39 (8): 1343–1357. Bibcode:2004M&PS...39.1343S. doi:10.1111/j.1945-5100.2004.tb00950.x.

External links

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