3040 Kozai
| Discovery | |
|---|---|
| Discovered by | W. Liller |
| Discovery site | Cerro Tololo |
| Discovery date | 23 January 1979 |
| Designations | |
| MPC designation | 3040 Kozai |
|
Named after
|
Yoshihide Kozai (astronomer) |
| 1979 BA | |
| Mars-crosser | |
| Orbital characteristics | |
| Epoch 16 February 2017 (JD 2457800.5) | |
| Uncertainty parameter 0 | |
| Observation arc | 37.24 yr (13,602 days) |
| Aphelion | 2.2096 AU |
| Perihelion | 1.4719 AU |
| 1.8407 AU | |
| Eccentricity | 0.2004 |
| 2.50 yr (912 days) | |
| 134.44° | |
| Inclination | 46.639° |
| 143.51° | |
| 290.21° | |
| Earth MOID | 0.6391 AU |
| Physical characteristics | |
| Dimensions | 4–11 km (conversion) |
| SMASS = S | |
| 13.8 | |
3040 Kozai, provisional designation 1979 BA, is a stony asteroid and Mars-crosser on a tilted orbit from the innermost regions of the asteroid belt, approximately 4 kilometers in diameters. It was discovered by American astronomer William Liller at Cerro Tololo Inter-American Observatory in Chile, on 23 January 1979. The asteroid is considered a classical example of an object submitted to the Kozai effect, induced by an outer perturber, which in this case is the gas giant Jupiter.
The S-type asteroid orbits the Sun at a distance of 1.5–2.2 AU once every 2 years and 6 months (912 days). Its orbit has an eccentricity of 0.20 and an inclination of 47° with respect to the ecliptic.of 1.5–2.2 AU once every 2 years and 6 months (912 days). Its orbit shows a notable eccentricity of 0.20. The orbit is also heavily inclined by 47 degrees to the plane of the ecliptic.
Little is known about the asteroids size, composition, albedo and rotation, despite having a well-observed orbit with the lowest possible uncertainty – which is denoted by a condition code of 0 – and an observation arc that spans over a time period of almost 40 years. With an absolute magnitude of 13.8, the asteroid's diameter could be anywhere between 4 and 11 kilometers for an assumed albedo in the range of 0.05–0.25 (see NASA's conversion table). Since the asteroid's spectral type is that of a brighter stony rather than a darker carbonaceous body, its diameter is on the lower end of NASA's generic conversion table, as the larger the body's diameter, the lower its albedo at a constant absolute magnitude.
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