| Discovery[1] | |
|---|---|
| Discovered by | K. Reinmuth |
| Discovery site | Heidelberg Obs. |
| Discovery date | 18 October 1931 |
| Designations | |
| (1235) Schorria | |
| Pronunciation | /ˈʃɒriə/ |
Named after | Richard Schorr[2] (1867–1951) (German astronomer) |
| 1931 UJ · 1988 HD | |
| Mars-crosser[3] · Hungaria[1][4] | |
| Orbital characteristics[3] | |
| Epoch 31 May 2020 (JD 2459000.5) | |
| Uncertainty parameter 0 | |
| Observation arc | 88.52yr (32,333 d) |
| Aphelion | 2.2056AU |
| Perihelion | 1.6147 AU |
| 1.9102 AU | |
| Eccentricity | 0.1547 |
| 2.64 yr (964 d) | |
| 183.19° | |
| 0° 22m 23.88s / day | |
| Inclination | 24.998° |
| 12.947° | |
| 43.732° | |
| Earth MOID | 0.6612 AU (257.6LD) |
| Physical characteristics | |
| 5.55±1.11 km[5] 9 km(estimate)[6] 11±4(generic)[7] | |
| 1265±25 h[6][a] | |
| 0.40(assumed)[4] 0.486±0.194[5] | |
| 12.68[3][5] 13.10[1][4][8][9] | |
1235 Schorria (prov. designation:1931 UJ), is aHungaria asteroid, sizableMars-crosser, and exceptionallyslow rotator from the inner region of theasteroid belt. The carbonaceousC-type asteroid has an outstandingly longrotation period of 1265 hours (7.5 weeks) and measures approximately 5.5 kilometers (3.4 miles) kilometers in diameter. It was discovered byKarl Reinmuth atHeidelberg Observatory in southwest Germany on 18 October 1931,[1] and named after German astronomerRichard Schorr (1867–1951).[2]
Schorria is aMars-crossing member of theHungaria asteroids, which form the innermost dense concentration ofasteroids in theSolar System. It orbits the Sun in theinner main-belt at a distance of 1.6–2.2 AU once every 2 years and 8 months (964 days;semi-major axis of 1.91 AU). Its orbit has aneccentricity of 0.15 and aninclination of 25° with respect to theecliptic.[3] The body'sobservation arc begins at Heidelberg two weeks after its official discovery observation, as noprecoveries were taken, and no prior identifications were made.[1]
Thisminor planet was named afterRichard Schorr (1867–1951), a German astronomer atBergedorf Observatory, Hamburg, who discovered the minor planets869 Mellena and1240 Centenaria. After being named byARI with the consent of the discoverer (RI 862), naming citation was later published byPaul Herget inThe Names of the Minor Planets in 1955 (H 114).[2] The lunar craterSchorr is also named in the astronomer's honour.[2] In 1913, asteroid725 Amanda was already named after Schorr's wife by discovering astronomerJohann Palisa.[10]
In theTholen taxonomy,Schorria'spectral type is closest to that of a carbonaceousC-type and somewhat similar to that of anX-type asteroid though with a noisy spectrum (CX:).[3]
In March 2009, a rotationallightcurve[a] ofSchorria was obtained fromphotometric observations by American astronomersBrian Warner andRobert 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 theslowest rotating asteroids known to exist. It has arotation period of1265±80 hours, or about 52 days, with a high brightness variation of1.40 inmagnitude (U=3),[6] 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.[6]
According to the space-based survey by NASA'sWide-field Infrared Survey Explorer with its subsequentNEOWISE mission,Schorria measures (5.55±1.11) kilometers in diameter and its surface has an albedo of (0.486±0.194).[5] Based on a generic magnitude-to-diameter conversion, the body measures between 7 and 15 kilometers, for anabsolute magnitude at 13 and an albedo in the range of 0.05 to 0.25,[7] while Warner/Stephens estimated a diameter of approximately 9 kilometers in 2009.[6]: 103
TheCollaborative Asteroid Lightcurve Link calculates a diameter of 5.04 kilometers based on an albedo of 0.40, which is contrary to an expected low albedo for dark, carbonaceous CX-type asteroids as classified by Tholen,[4] but typical for the descendants of theE-belt, a hypothesized population of primordial asteroids, which theE-type Hungarian asteroids with high inclinations and a semi-major axis of 1.9 AU are thought to have originated from.[4]
