1985 Hopmann

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1985 Hopmann (prov. designation: Template:Mp) is a dark background asteroid in the outer regions of the asteroid belt. It was discovered on 13 January 1929, by astronomer Karl Reinmuth at Landessternwarte Heidelberg-Königstuhl in southern Germany.[1] The asteroid has a rotation period of 17.5 hours and measures approximately Script error: No such module "convert". in diameter. It was later named after German astronomer Josef Hopmann (1890–1975).[2]

Orbit and classification

Hopmann is a dark C-type asteroid that orbits the Sun in the outer main-belt at a distance of 2.6–3.6 AU once every 5 years and 6 months (2,014 days). Its orbit has an eccentricity of 0.15 and an inclination of 17° with respect to the ecliptic.[3] The first observation used for the body's observation arc was taken at the discovering observatory on 4 February 1926, or 22 days after its official discovering observation.[1]

Naming

This minor planet was named in memory of German astronomer Josef Hopmann (1890–1975), a director of Vienna Observatory between 1951 and 1962, a productive observer of variable and binary stars, and a participant in the international program to observe near-Earth asteroid 433 Eros in the early 1930s. The lunar crater Hopmann is also named in his honour.[2] The official Template:MoMP was published by the Minor Planet Center on 15 October 1977 (M.P.C. 4237Script error: No such module "Check for unknown parameters".).[4]

Physical characteristics

According to the survey carried out by the Infrared Astronomical Satellite IRAS, Hopmann measures 35.51 kilometers in diameter.[3] The Collaborative Asteroid Lightcurve Link agrees with the Supplemental IRAS Minor Planet Survey (SIMPS) data and derives an albedo of 0.039 and a diameter of 35.47 kilometers,[5] while observations with NASA's Wide-field Infrared Survey Explorer and its subsequent NEOWISE mission gave an albedo of 0.06 and a diameter of 44.33 kilometers.[6]

In January and February 2012, three rotational lightcurves were obtained by Robert Stephens at Santana Observatory (646Script error: No such module "Check for unknown parameters".), California, Josep Maria Aymami at Carmelita Observatory (B20Script error: No such module "Check for unknown parameters".), Barcelona, and Patricia Moravec at Oakley Southern Sky Observatory (E09Script error: No such module "Check for unknown parameters".), Australia. The lightcurves gave a well-defined rotation period of 17.476, 17.478 and 17.480 hours, respectively, with a brightness variation between 0.36 and 0.44 magnitude (U=3/3/3-Script error: No such module "Check for unknown parameters".).[7][8][9] In 2016, a re-modeled lightcurve, constructed from data compiled in the Lowell Photometric Database, also gave a concurring period.[10]

References

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External links

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