1235 Schorria
| Discovery | |
|---|---|
| Discovered by | K. Reinmuth |
| Discovery site | Heidelberg Obs. |
| Discovery date | 18 October 1931 |
| Designations | |
| MPC designation | (1235) Schorria |
|
Named after
|
Richard Schorr (astronomer) |
| 1931 UJ · 1988 HD | |
| Mars-crosser · Hungaria | |
| Orbital characteristics | |
| Epoch 16 February 2017 (JD 2457800.5) | |
| Uncertainty parameter 0 | |
| Observation arc | 85.23 yr (31,130 days) |
| Aphelion | 2.2053 AU |
| Perihelion | 1.6155 AU |
| 1.9104 AU | |
| Eccentricity | 0.1544 |
| 2.64 yr (964 days) | |
| 95.224° | |
| 0° 22m 23.88s / day | |
| Inclination | 25.003° |
| 12.961° | |
| 43.713° | |
| Earth MOID | 0.6623 AU |
| Physical characteristics | |
| Dimensions | 5.04 km (calculated) 9 km (estimate) 11±4 (generic) |
|
3.3±0.02 h (incorrect) 1265±25 h |
|
| 0.40 (assumed) | |
|
B–V = 0.750 U–B = 0.330 Tholen = CX: · CX: |
|
| 12.68 · 12.71±0.63 · 13.10±0.04 | |
1235 Schorria, provisional designation 1931 UJ, is a Hungaria asteroid, sizable Mars-crosser, and exceptionally slow rotator from the inner region of the asteroid belt, approximately 5 kilometers in diameter. It was discovered on 18 October 1931, by German astronomer Karl Reinmuth at Heidelberg Observatory in southwest Germany, and named for astronomer Richard Schorr.
In the Tholen taxonomy, Schorria is classified as a CX:-type, an intermediate between the C-type and X-type asteroids. It is a member of the Hungaria family, which form the innermost dense concentration of asteroids in the Solar System. It orbits the Sun at a distance of 1.6–2.2 AU once every 2 years and 8 months (964 days). Its orbit has an eccentricity of 0.15 and an inclination of 25° with respect to the ecliptic. The body's observation arc begins at Heidelberg two weeks after its official discovery observation, as no precoveries were taken, and no prior identifications were made.
In March 2009, a rotational light-curve of Schorria was obtained by American astronomers Brian Warner and Robert Stephens. Light curve analysis of the two astronomer's combined data set of almost 2000 photometric observations revealed that this Mars-crosser is one of the slowest rotating asteroids known to exist. It has a rotation period of 1265±80 hours, or about 52 days, with a high brightness variation of 1.40 in magnitude (U=3), which is indicative of a non-spheroidal shape. The body was also suspected to be in a tumbling state. However, no significant evidence of such a non-principal axis rotation could be found.
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