| Minorplanet: | yes |
| 927 Ratisbona | |
| Background: |
|
| Discovery Ref: |   |
| Discovered: | 16 February 1920 |
| Mpc Name: | (927) Ratisbona |
| Alt Names: | A920 DB1920 GO 1958 VD1958 XQ |
| Named After: | Regensburg |
| Mp Category: | main-belt   background  |
| Orbit Ref: |   |
| Epoch: | 31 May 2020 (JD 2459000.5) |
| Uncertainty: | 0 |
| Observation Arc: | 99.57 yr (36,368 d) |
| Perihelion: | 2.9476 AU |
| Semimajor: | 3.2285 AU |
| Eccentricity: | 0.0870 |
| Period: | 5.80 yr (2,119 d) |
| Mean Motion: | / day |
| Inclination: | 14.572° |
| Asc Node: | 7.6887° |
| Arg Peri: | 171.36° |
| Mean Diameter: | |
| Albedo: | |
| Spectral Type: | |
| Abs Magnitude: | 9.3 |
927 Ratisbona is a large and dark background asteroid, approximately 76km (47miles) in diameter, located in the outer region of the asteroid belt. It was discovered on 16 February 1920, by astronomer Max Wolf at the Heidelberg Observatory in southwest Germany. The carbonaceous C-type asteroid (CB) has a rotation period of 12.99 hours and is rather spherical in shape. It was named after the Bavarian city of Regensburg.
Ratisbona is a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements. It orbits the Sun in the outer asteroid belt at a distance of 2.9–3.5 AU once every 5 years and 10 months (2,119 days; semi-major axis of 3.23 AU). Its orbit has an eccentricity of 0.09 and an inclination of 15° with respect to the ecliptic. The body's observation arc begins at Heidelberg-Königstuhl State Observatory on 17 February 1920, the night after its official discovery observation.
This minor planet was named after the Latin name of the German city of Regensburg in Bavaria, where astronomer Johannes Kepler died in 1630. The was mentioned in the astronomical journal Astronomische Nachrichten in 1930 .
In the Tholen classification, Ratisbona is most similar to a common, carbonaceous C-type asteroid, and somewhat similar to a brighter B-type asteroid, based on a nosy spectrum (CB:).
Over the course of seven nights in January 2018, a rotational lightcurve of Ratisbona was obtained from photometric observations by Tom Polakis at the Command Module Observatory in Arizona. Lightcurve analysis gave a rotation period of hours with a low brightness variation of magnitude, indicative of a regular, spherical shape . The result supersedes a period of hours with an amplitude of magnitude determined by René Roy, Raoul Behrend, Pierre Antonini and Donn Starkey in October 2004 .
According to the survey carried out by the Infrared Astronomical Satellite IRAS, the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), and the Japanese Akari satellite, Ratisbona measures, and kilometers in diameter and its surface has a very low albedo of, and, respectively.
The Collaborative Asteroid Lightcurve Link adopts the results from IRAS, that is, a albedo of 0.0591 and a diameter of 67.57 km based on an absolute magnitude of 9.54. Further published mean-diameters and albedos by the WISE team include and and albedos of and . An asteroid occultation, observed on 13 September 2014, gave a best-fit ellipse dimension of 78.0 × 78.0 kilometers. These timed observations are taken when the asteroid passes in front of a distant star. However the quality of the measurement is rated poorly.