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° | |
| Inclination | 7.6293° |
| 351.78° | |
| 247.22° | |
| Earth MOID | 1.26459 AU (189.180 Gm) |
| Jupiter MOID | 2.43888 AU (364.851 Gm) |
| 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
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- ↑ 2.0 2.1 Lua error in package.lua at line 80: module 'strict' not found.
- ↑ 3.0 3.1 3.2 3.3 Lua error in package.lua at line 80: module 'strict' not found.
- ↑ 4.0 4.1 4.2 Lua error in package.lua at line 80: module 'strict' not found.
- ↑ 5.0 5.1 5.2 Lua error in package.lua at line 80: module 'strict' not found.
- ↑ 6.0 6.1 6.2 Lua error in package.lua at line 80: module 'strict' not found.
- ↑ 7.0 7.1 Lua error in package.lua at line 80: module 'strict' not found.
- ↑ Lua error in package.lua at line 80: module 'strict' not found.
- ↑ Lua error in package.lua at line 80: module 'strict' not found.
External links
- Asteroid Lightcurve Database (LCDB), query form (info)
- Dictionary of Minor Planet Names, Google books
- Asteroids and comets rotation curves, CdR – Observatoire de Genève, Raoul Behrend
- Discovery Circumstances: Numbered Minor Planets (1)-(5000) – Minor Planet Center
- 1998 Titius at the JPL Small-Body Database
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