(575) Renata ( lat. Renate ) - an asteroid of the main belt , which is part of the family of Mary [1] . It was discovered on September 19, 1905 by the German astronomer Max Wolf at the Heidelberg Observatory in Germany .
| (575) Renata | |
|---|---|
| Asteroid | |
| Opening | |
| Discoverer | Max wolf |
| Detection point | Heidelberg |
| Date of discovery | September 19, 1905 |
| Alternative designations | 1905 RE ; 1981 EO 1 |
| Category | Asteroid belt ( Maria's family ) |
| Orbital characteristics | |
| The era of December 9, 2014 JD 2457000.5 | |
| Eccentricity ( e ) | 0.1278817 |
| Semi-axis ( a ) | 382.137 million km (2.5544289 a. E.) |
| Perihelion ( q ) | 333.269 million km (2,2277642 a. E.) |
| Afhelia ( Q ) | 431.005 million km (2.8810936 a. E.) |
| Period of circulation ( P ) | 1491,211 days (4.083 g. ) |
| Average orbital speed | 18,559 km / s |
| Inclination ( i ) | 15,01144 ° |
| Ascending node longitude (Ω) | 349.68619 ° |
| Perihelion Argument (ω) | 334.07405 ° |
| Mean Anomaly ( M ) | 295.57365 ° |
| physical characteristics | |
| Diameter | 21.26 km |
| Rotation period | 3,676 h |
| Apparent magnitude | 13.57 m (current) |
| Absolute magnitude | 10.7 m |
| Albedo | 0.1706 |
| Current distance from the Sun | 2,242 a. e. |
| Current distance from Earth | 1.262 a. e. |
The orbit of Renat asteroid and its position in the solar system
Photometric observations made at the Colorado Springs Observatory in 1999 made it possible to obtain the light curves of this body, from which it followed that the period of rotation of the asteroid around its axis is equal to 3.676 ± 0.002 hours, with a change in brightness as it turns 0.15 ± 0.01 m [2] .
See also
- List of asteroids ( 501–600 )
- Small Planet Classifications
- Maria's family
Notes
- ↑ Veeder, GJ; Matson, DL; Owensby, PD & Gradie, JC (March 1995), Eos, Koronis, and Maria asteroids family: Infrared (JHK) photometry , vol. 114, p. 186–196 , DOI 10.1006 / icar.1995.1053
- ↑ Warner, Brian D. (January 2011), Upon Further Review: IV. An Examination of Lightcurve Analysis from the Palmer Divide Observatory , vol. 38, p. 52–54