| Minorplanet: | yes |
| 1077 Campanula | |
| Background: |
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| Discovered: | 6 October 1926 |
| Mpc Name: | (1077) Campanula |
| Alt Names: | 1926 TK1957 AJ 1972 CB |
| Epoch: | 4 September 2017 (JD 2458000.5) |
| Uncertainty: | 0 |
| Observation Arc: | 90.56 yr (33,077 days) |
| Perihelion: | 1.9220 AU |
| Semimajor: | 2.3938 AU |
| Eccentricity: | 0.1971 |
| Period: | 3.70 yr (1,353 days) |
| Mean Motion: | / day |
| Inclination: | 5.3941° |
| Asc Node: | 346.20° |
| Arg Peri: | 13.591° |
| Mean Diameter: | km km km |
| Rotation: | |
| Pole Ecliptic Lat: |
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| Albedo: | |
| Spectral Type: | SV–R = |
| Abs Magnitude: | 12.3 |
1077 Campanula, provisional designation, is a presumed Erigonian asteroid, approximately 9abbr=offNaNabbr=off in diameter, located in the inner region of the asteroid belt. It was discovered on 6 October 1926, by German astronomer Karl Reinmuth at the Heidelberg Observatory in southwest Germany. The asteroid was named after the bellflower Campanula.
Campanula is considered to be a member of the Erigone family, which is named after 163 Erigone, while other sources classify it as a background asteroid, not associated to any known asteroid family. It orbits the Sun in the inner main-belt at a distance of 1.9–2.9 AU once every 3 years and 8 months (1,353 days). Its orbit has an eccentricity of 0.20 and an inclination of 5° with respect to the ecliptic. The body's observation arc begins at Heidelberg, 2 months after its official discovery observation.
This minor planet was named for the bellflower Campanula. The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 .
Due to his many discoveries, Karl Reinmuth submitted a large list of 66 newly named asteroids in the early 1930s. The list covered his discoveries with numbers between and . This list also contained a sequence of 28 asteroids, starting with 1054 Forsytia, that were all named after plants, in particular flowering plants (also see list of minor planets named after animals and plants).
Campanula is an assumed stony S-type asteroid, which is not in line with the darker C- and X-types seen among the Erigonian asteroids.
Several rotational lightcurves of Campanula were obtained from photometric observations. Lightcurve analysis gave a rotation period of 3.847 to 3.852 hours with a brightness variation of 0.24 to 0.40 magnitude . A 2016-published lightcurve, using modeled photometric data from the Lowell Photometric Database (LPD), gave a concurring period of 3.850486 hours, as well as two spin axis of (178.0°, 76.0°) and (313.0°, 59.0°) in ecliptic coordinates (λ, β).
According to observations taken at the Balzaretto Observatory and the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Campanula measures between 7.55 and 9.709 kilometers in diameter and its surface has an albedo between 0.225 and 0.33. The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 9.40 kilometers based on an absolute magnitude of 12.50.