1775 Zimmerwald
| Discovery | |
|---|---|
| Discovered by | P. Wild |
| Discovery site | Zimmerwald Obs. |
| Discovery date | 13 May 1969 |
| Designations | |
| MPC designation | (1775) Zimmerwald |
|
Named after
|
Zimmerwald (village; observatory) |
| 1969 JA · 1952 HB2 1952 HD · 1953 TE2 |
|
| main-belt · Eunomia | |
| Orbital characteristics | |
| Epoch 16 February 2017 (JD 2457800.5) | |
| Uncertainty parameter 0 | |
| Observation arc | 67.13 yr (24,519 days) |
| Aphelion | 3.0865 AU |
| Perihelion | 2.1188 AU |
| 2.6026 AU | |
| Eccentricity | 0.1859 |
| 4.20 yr (1,534 days) | |
| 101.59° | |
| 0° 14m 4.92s / day | |
| Inclination | 12.555° |
| 195.94° | |
| 84.735° | |
| Physical characteristics | |
| Dimensions |
10.17±0.69 km 10.232±0.088 km 10.70±2.19 km 11.03 km (calculated) |
| 122±5 h | |
|
0.21 (assumed) 0.21±0.09 0.244±0.041 0.247±0.035 |
|
| S | |
| 12.08±0.31 · 12.1 · 12.26 | |
1775 Zimmerwald, provisional designation 1969 JA, is a stony Eunomian asteroid and slow rotator from the middle region of the asteroid belt, approximately 10 kilometers in diameter. It was discovered on 13 May 1969, by Swiss astronomer Paul Wild at Zimmerwald Observatory near Bern, Switzerland. It is named for the village of Zimmerwald, where the discovering observatory is located.
Zimmerwald is a member of the Eunomia family, a large group of mostly stony S-type asteroids and the most prominent family in the intermediate main-belt, which is located between two prominent Kirkwood gaps. It orbits the Sun at a distance of 2.1–3.1 AU once every 4 years and 2 months (1,534 days). Its orbit has an eccentricity of 0.19 and an inclination of 13° with respect to the ecliptic. The first precovery of Zimmerwald was taken at Palomar Observatory in 1949, extending the body's observation arc by 20 years prior to its official discovery observation at Zimmerwald. During the 1950s, it was also identified at Heidelberg, Goethe Link and McDonald Observatory.
In May 2011, a rotational lightcurve of Zimmerwald was obtained by American astronomer Robert Stephens at the Center for Solar System Studies, California, using photometric observations taken at the Santana and Goat Mountain observatories (646, G79). Lightcurve analysis gave a very long rotation period of 122±5 hours with a change in brightness of 0.60 magnitude (U=2+). It is also suspected, that the body might be in a nonprincipal axis rotation, which is commonly known as "tumbling". While the slowest rotators have periods above 1000 hours, the majority of minor planets have periods shorter than 20 hours.
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