1998 Titius

1998 Titius
Discovery [1]
Discovered by A. Bohrmann
Discovery site Heidelberg Obs.
Discovery date 24 February 1938
Designations
MPC designation 1998 Titius
Named after
 Johann Titius
(astronomer)[2]
1938 DX1 · 1966 TF
main-belt · (inner) [3]
Orbital characteristics [1]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 0
Observation arc 78.06 yr (28511 days)
Aphelion 2.5738 AU (385.03 Gm)
Perihelion 2.2637 AU (338.64 Gm)
2.4187 AU (361.83 Gm)
Eccentricity 0.064094
3.76 yr (1374.0 d)
177.40°
0° 15m 43.236s / day
Inclination 7.6293°
351.78°
247.22°
Earth MOID 1.26459 AU (189.180 Gm)
Jupiter MOID 2.43888 AU (364.851 Gm)
Jupiter Tisserand parameter 3.500
Physical characteristics
Dimensions 15.98±0.35 km[4]
14.782±0.081 km[5]
14.24±0.17 km[6]
10.79 km (calculated)[3]
6.13±0.01 h,[7] 6.13 h (0.255 d)[1]
0.093±0.004[4]
0.1066±0.0037[5]
0.126±0.031[6]
0.20 (assumed)[3]
SMASS = Xc
X [3]
12.2[1]

    1998 Titius, provisional designation 1938 DX1, is a transitional metallic–carbonaceous asteroid from the inner regions of the asteroid belt, about 14 kilometers in diameter. It was discovered on 24 February 1938, by German astronomer Alfred Bohrmann at Heidelberg Observatory in southern Germany.[8]

    The asteroid orbits the Sun at a distance of 2.3–2.6 AU once every 3 years and 9 months (1,374 days) and stays in a 2:1 orbital resonance with the planet Mars.[9] Its orbit is tilted by 8 degrees to the plane of the ecliptic and shows a low eccentricity of 0.06. According to observations carried out by the Akari and Wide-field Infrared Survey Explorer satellites, it has an albedo between 0.09 and 0.11.[4][5][6] Its spectral classification is that of a Xc-type asteroid in the SMASS taxonomy, a transitional spectral type between the two large main groups of metallic X-type and carbonaceous C-type asteroids. Both types are much darker than the stony S-type asteroids, which are also very common in the inner main-belt.

    Based upon photometric measurements made at the Californian Santana Observatory, the body has a rotation period of 6.13±0.01 hours, during which its brightness amplitude varies by 0.30±0.04 magnitude.[7]

    It is named after German astronomer Johann Daniel Titius (1729–1796), best known for formulating the Titius-Bode law, which states that each subsequent planet in the Solar System is roughly twice as far from the Sun than the previous one. He is also honored by the lunar crater Titius.[2]

    References

    1. 1 2 3 4 "JPL Small-Body Database Browser: 1998 Titius (1938 DX1)" (2015-11-18 last obs.). Jet Propulsion Laboratory. Retrieved 17 April 2016.
    2. 1 2 Schmadel, Lutz D. (2003). Dictionary of Minor Planet Names – (1998) Titius. Springer Berlin Heidelberg. p. 162. ISBN 978-3-540-29925-7. Retrieved 15 December 2015.
    3. 1 2 3 4 "LCDB Data for (1998) Titius". Asteroid Lightcurve Database (LCDB). Retrieved 15 December 2015.
    4. 1 2 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. Bibcode:2011PASJ...63.1117U. doi:10.1093/pasj/63.5.1117. Retrieved 15 December 2015.
    5. 1 2 3 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:1109.6407Freely accessible. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. Retrieved 15 December 2015.
    6. 1 2 3 Masiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Nugent, C.; Cabrera, M. S. (November 2012). "Preliminary Analysis of WISE/NEOWISE 3-Band Cryogenic and Post-cryogenic Observations of Main Belt Asteroids". The Astrophysical Journal Letters. 759 (1): 5. arXiv:1209.5794Freely accessible. Bibcode:2012ApJ...759L...8M. doi:10.1088/2041-8205/759/1/L8. Retrieved 15 December 2015.
    7. 1 2 Stephens, R. D. (September 2002). "Photometry of 973 Aralia, 1189 Terentia, 1040 Klumpkea, and 1998 Titius". The Minor Planet Bulletin. 29: 47–48. Bibcode:2002MPBu...29...47S. Retrieved 15 December 2015.
    8. ↑ "1998 Titius (1938 DX1)". Minor Planet Center. Retrieved 15 December 2015.
    9. ↑ Gallardo, Tabaré; Venturini, Julia; Roig, Fernando; Gil-Hutton, Ricardo (August 2011). "Origin and sustainability of the population of asteroids captured in the exterior resonance 1:2 with Mars". Icarus. 214 (2): 632–644. arXiv:1105.5108Freely accessible. Bibcode:2011Icar..214..632G. doi:10.1016/j.icarus.2011.05.029. Retrieved 15 December 2015.

    External links


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