1929 Kollaa
| Discovery | |
|---|---|
| Discovered by | Y. Väisälä |
| Discovery site | Turku Obs. |
| Discovery date | 20 January 1939 |
| Designations | |
| MPC designation | (1929) Kollaa |
|
Named after
|
Kollaa River (in Karelia) |
| 1939 BS · 1939 CH 1943 GG · 1968 BH 1976 JF3 |
|
| main-belt · Vestian | |
| Orbital characteristics | |
| Epoch 16 February 2017 (JD 2457800.5) | |
| Uncertainty parameter 0 | |
| Observation arc | 48.38 yr (17,672 days) |
| Aphelion | 2.5396 AU |
| Perihelion | 2.1854 AU |
| 2.3625 AU | |
| Eccentricity | 0.0750 |
| 3.63 yr (1,326 days) | |
| 172.30° | |
| 0° 16m 17.04s / day | |
| Inclination | 7.7798° |
| 65.433° | |
| 71.236° | |
| Physical characteristics | |
| Dimensions | 6.06 km (calculated) 6.71±0.34 km 7.772±0.147 km |
|
2.980±0.005 h 2.9887±0.0004 h |
|
|
0.3855±0.0958 0.393±0.066 0.4 (assumed) |
|
| SMASS = V · V | |
| 12.2 · 12.50 · 12.6 · 12.64±0.32 · 12.7 | |
1929 Kollaa, provisional designation 1939 BS, is a stony Vestian asteroid from the inner regions of the asteroid belt, approximately 7 kilometers in diameter. It was discovered by Finnish astronomer Yrjö Väisälä at Turku Observatory in Southwest Finland, on 20 January 1939.
The bright V-type asteroid is a member of the Vesta family. Vestian asteroids have a composition akin to cumulate eucrite meteorites and are thought to have originated deep within 4 Vesta's crust, possibly from the Rheasilvia crater, a large impact crater on its southern hemisphere near the South pole, formed as a result of a subcatastrophic collision. The asteroid Vesta is the main-belt's second-most-massive body after 1 Ceres.
1929 Kollaa orbits the Sun at a distance of 2.2–2.5 AU once every 3 years and 8 months (1,326 days). Its orbit has an eccentricity of 0.08 and an inclination of 8° with respect to the ecliptic. As no precoveries were taken, the asteroid's observation arc begins with its discovery.
It has a well-defined rotation period of 2.98 hours, derived from two rotational light-curve analysis. In March 2004, photometric observations at the U.S. Magdalena Ridge Observatory in New Mexico rendered a period of 2.980±0.005 hours with a brightness variation of 0.20 in magnitude (U=3). In 2008 a second, concurring period was obtained by French amateur astronomer Pierre Antonini at his private Observatoire de Bédoin in France (132). It gave a period of 2.9887±0.0004 hours and an amplitude 0.22 in magnitude (U=3).
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