1235 Schorria

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1235 Schorria
Discovery [1]
Discovered by K. Reinmuth
Discovery site Heidelberg Obs.
Discovery date 18 October 1931
MPC designation (1235) Schorria
Named after
Richard Schorr (astronomer)[2]
1931 UJ · 1988 HD
Mars-crosser[1] · Hungaria[3][4]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 85.70 yr (31,303 days)
Aphelion 2.2056 AU
Perihelion 1.6153 AU
1.9104 AU
Eccentricity 0.1545
2.64 yr (964 days)
0° 22m 23.88s / day
Inclination 25.001°
Physical characteristics
Dimensions 5.04 km (calculated)[4]
5.55±1.11 km[5]
9 km (estimate)[6]
11±4 (generic)[7]
3.3±0.02 h (incorrect)[8]
1265±25 h[6][a]
0.40 (assumed)[4]
Tholen = CX: [1] · CX: [4]
B–V = 0.750[1]
U–B = 0.330[1]
12.68[1][5] · 12.71±0.63[9] · 13.10±0.04[4][10][11]

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 5.5 kilometers in diameter. It was discovered on 18 October 1931, by German astronomer Karl Reinmuth at Heidelberg Observatory in southwest Germany,[3] and named for astronomer Richard Schorr.[2]

Orbit and classification[edit]

Schorria is a Mars-crossing member of the Hungaria family, which form the innermost dense concentration of asteroids in the Solar System. It orbits the Sun in the inner main-belt 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.[1] 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.[3]

Physical characteristics[edit]

In the Tholen taxonomy, Schorria is classified as a CX:-type, an intermediate between the C-type and X-type asteroids.

Slow rorator[edit]

In March 2009, a rotational lightcurve[a] 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),[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]

Diameter and albedo[edit]

According to the space-based survey by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Schorria measures 5.55 kilometers in diameter and its surface has an albedo of 0.486.[5]

Based on a generic magnitude-to-diameter conversion, the body measures between 7 and 15 kilometers, for an absolute 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

The Collaborative 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 the E-belt, a hypothesized population of primordial asteroids, which the E-type Hungarian asteroids with high inclinations and a semi-major axis of 1.9 AU are thought to have originated from.[4]


This minor planet was named after Richard Schorr (1867–1951), astronomer at Bergedorf Observatory, Hamburg, who discovered the minor planets 869 Mellena and 1240 Centenaria. After being named by ARI with the consent of the discoverer (RI 862), naming citation was later published by Paul Herget in The Names of the Minor Planets in 1955 (H 114).[2] The lunar crater Schorr is also named in the astronomer's honour.[2]


  1. ^ a b Lightcurve plot of (1235) Schorria, Palmer Divide Observatory, B. D. Warner (2009)


  1. ^ a b c d e f g h "JPL Small-Body Database Browser: 1235 Schorria (1931 UJ)" (2017-07-01 last obs.). Jet Propulsion Laboratory. Retrieved 26 July 2017. 
  2. ^ a b c d Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (1235) Schorria. Springer Berlin Heidelberg. p. 103. ISBN 978-3-540-00238-3. Retrieved 25 January 2017. 
  3. ^ a b c "1235 Schorria (1931 UJ)". Minor Planet Center. Retrieved 25 January 2017. 
  4. ^ a b c d e f g "LCDB Data for (1235) Schorria". Asteroid Lightcurve Database (LCDB). Retrieved 25 January 2017. 
  5. ^ a b c d Alí-Lagoa, V.; Delbo', M. (July 2017). "Sizes and albedos of Mars-crossing asteroids from WISE/NEOWISE data" (PDF). Astronomy and Astrophysics. 603: 8. arXiv:1705.10263Freely accessible. Bibcode:2017A&A...603A..55A. doi:10.1051/0004-6361/201629917. Retrieved 20 October 2017. 
  6. ^ a b c d e Warner, Brian D.; Stephens, Robert D. (July 2009). "The Lightcurve for the Long-Period Hungaria Asteroid 1235 Schorria". The Minor Planet Bulletin. 36 (3): 102–103. Bibcode:2009MPBu...36..102W. ISSN 1052-8091. Retrieved 25 January 2017. 
  7. ^ a b "Absolute Magnitude (H)". NASA/JPL. Retrieved 26 January 2017. 
  8. ^ Behrend, Raoul. "Asteroids and comets rotation curves – (1235) Schorria". Geneva Observatory. Retrieved 25 January 2017. 
  9. ^ Veres, Peter; Jedicke, Robert; Fitzsimmons, Alan; Denneau, Larry; Granvik, Mikael; Bolin, Bryce; et al. (November 2015). "Absolute magnitudes and slope parameters for 250,000 asteroids observed by Pan-STARRS PS1 – Preliminary results". Icarus. 261: 34–47. arXiv:1506.00762Freely accessible. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. Retrieved 25 January 2017. 
  10. ^ Wisniewski, W. Z.; Michalowski, T. M.; Harris, A. W.; McMillan, R. S. (March 1995). "Photoelectric Observations of 125 Asteroids". Abstracts of the Lunar and Planetary Science Conference. Bibcode:1995LPI....26.1511W. Retrieved 25 January 2017. 
  11. ^ Pravec, Petr; Harris, Alan W.; Kusnirák, Peter; Galád, Adrián; Hornoch, Kamil (September 2012). "Absolute magnitudes of asteroids and a revision of asteroid albedo estimates from WISE thermal observations". Icarus. 221 (1): 365–387. Bibcode:2012Icar..221..365P. doi:10.1016/j.icarus.2012.07.026. Retrieved 25 January 2017. 

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