(10313) Vanessa-Mae
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Asteroid (10313) Vanessa-Mae |
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| Properties of the orbit ( animation ) | |
| Orbit type | Inner main belt asteroid |
| Major semi-axis | 2.2635 AU |
| eccentricity | 0.2118 |
| Perihelion - aphelion | 1.7841 AU - 2.7430 AU |
| Inclination of the orbit plane | 4.6618 ° |
| Length of the ascending node | 288.4315 ° |
| Argument of the periapsis | 71.4880 ° |
| Time of passage of the perihelion | June 21, 2021 |
| Sidereal period | 3.41 a |
| Mean orbital velocity | 19.57 km / s |
| Physical Properties | |
| Medium diameter | 2.639 (± 0.421) km |
| Albedo | 0.440 (± 0.140) |
| Absolute brightness | 14.6 mag |
| history | |
| Explorer | Lyudmyla Shuravlowa |
| Date of discovery | August 26, 1990 |
| Another name | 1990 QW 17 , 1973 RH, 1994 WV 12 |
| Source: Unless otherwise stated, the data comes from JPL Small-Body Database Browser . The affiliation to an asteroid family is automatically determined from the AstDyS-2 database . Please also note the note on asteroid items. | |
(10313) Vanessa-Mae is an asteroid located in the inner main belt . It was discovered on August 26, 1990 by the Ukrainian astronomer Lyudmyla Shuravlowa at the Crimean Observatory in Nautschnyj ( IAU code 095). The asteroid had already been sighted at the Crimean Observatory: on September 2, 1973 under the provisional designation 1973 RH.
The mean diameter of the asteroid was roughly calculated to be 2.639 (± 0.421) kilometers. The albedo of 0.440 (± 0.140) indicates a light surface. According to the SMASS classification ( Small Main-Belt Asteroid Spectroscopic Survey ), a spectroscopic study by Gianluca Masi , Sergio Foglia and Richard P. Binzel subdivided all investigated asteroids into C, S and V types (10313) Vanessa -Mae assigned to the S asteroids .
Mean solar distance ( major semi-axis ), eccentricity, and inclination of the orbit plane of (10313) Vanessa-Mae roughly resemble the orbital data of members of the Flora family, a large group of asteroids named after (8) Flora . Asteroids of the Flora family move in a 4: 9 orbital resonance with the planet Mars around the sun . The group is also called the Ariadne family after the asteroid (43) Ariadne .
The rotation period of (10313) Vanessa-Mae was examined by Brian D. Warner in 2009 and 2019 and by David Higgins in 2011. However, the light curves were not sufficient for a determination.
(10313) Vanessa-Mae was named on March 18, 2003 after the violinist Vanessa-Mae (* 1978). The Venus craters Vanessa and Mae, however, were named in 1997 after the corresponding Greek first names.
Web links
- (10313) Vanessa-Mae in the database of the "Asteroids - Dynamic Site" (AstDyS-2, English).
- (10313) Vanessa-Mae in the Small-Body Database of the Jet Propulsion Laboratory of NASA at the California Institute of Technology (Caltech) in Pasadena , California (English)
- Discovery Circumstances by (10313) Vanessa-Mae according to the Minor Planet Center of the International Astronomical Union at the Harvard-Smithsonian Center for Astrophysics in Cambridge , Massachusetts (English)
Individual evidence
- ↑ (10313) Vanessa-Mae at the IAU Minor Planet Center (English)
- ^ Gianluca Masi, Sergio Foglia, Richard P. Binzel: Search for Unusual Spectroscopic Candidates Among 40313 minor planets from the 3rd Release of the Sloan Digital Sky Survey Moving Object Catalog . (English)
- ↑ subdivision of asteroids to S-types, C-types and V-types (English)
- ↑ The Venus crater Vanessa in the Gazetteer of Planetary Nomenclature of the IAU (WGPSN) / USGS (English)
- ↑ The Venus crater Mae in the Gazetteer of Planetary Nomenclature of the IAU (WGPSN) / USGS (English)