795 Fini (prov. designation: or ) is a dark and large background asteroid, approximately in diameter, located in the central region of the asteroid belt. It was discovered by Austrian astronomer Johann Palisa at the Vienna Observatory on 26 September 1914. The carbonaceous C-type asteroid has a poorly determined rotation period of 9.3 hours and seems rather spherical in shape. Any reference of the asteroid's name to a person is unknown. Orbit and classification Fini 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 central main-belt at a distance of 2.5–3.0 AU once every 4 years and 7 months (1,665 days; semi-major axis of 2.75 AU). Its orbit has an eccentricity of 0.10 and an inclination of 19° with respect to the ecliptic. The body's observation arc begins at Vienna Observatory on 16 March 1917, where it was officially discovered two and a half years before. Naming "Fini" is an Austrian diminutive of Josephine. Any reference of this minor planet name to a person or occurrence is unknown. Unknown meaning Among the many thousands of named minor planets, Fini is one of 120 asteroids for which no official naming citation has been published. All of these asteroids have low numbers, the first being . The last asteroid with a name of unknown meaning is . They were discovered between 1876 and the 1930s, predominantly by astronomers Auguste Charlois, Johann Palisa, Max Wolf and Karl Reinmuth. Physical characteristics In the Tholen classification, Fini is a common, carbonaceous C-type asteroid. It is also a C-type in the taxonomic classification based on near-infrared colors from the MOVIS-catalog, which was created from data gathered by the VISTA Hemisphere Survey conducted with the VISTA telescope at Paranal Observatory in Chile. Rotation period Several rotational lightcurves of Fini have been obtained from photometric observations. However, the asteroid, which shows a notably low brightness variation – indicative of a spherical rather than elongated shape – still has a poorly determined rotation period. Based on observations from February 2003 and November 2011, Brian Warner at his Palmer Divide Observatory in Colorado, determined three possible period solutions of , and hours with corresponding low amplitudes of , and magnitude (). Petr Pravec and Peter Kušnirák at Ondřejov Observatory derive a rotation period of hours from their observations in October 2001, or