(171) Ophelia ( Latin Ophelia ) is a rather large asteroid of the main belt , belonging to the dark spectral class C , consisting probably of the simplest carbon compounds similar to chondrite meteorites found on Earth and is part of the Themis family . The asteroid was discovered on January 13, 1877 by the French astronomer Alphonse Borelli at the Marseille Observatory and is named after Ophelia, a fictional character in the tragedy of William Shakespeare 's Hamlet .
| (171) Ophelia | |
|---|---|
| Opening | |
| Discoverer | Alphonse Borelli |
| Detection point | Marseilles |
| Date of discovery | January 13, 1877 |
| Category | Main ring ( Themis Family ) |
| Orbital characteristics | |
| The Age of March 14, 2012 JD 2456000.5 | |
| Eccentricity ( e ) | 0.13018 |
| Semi-axis ( a ) | 468.554 million km (3.13209 a. E.) |
| Perihelion ( q ) | 407.558 million km (2,72435 a. E.) |
| Afhelia ( Q ) | 529.55 million km (3,53983 a. E.) |
| Period of circulation ( P ) | 2024,649 days (5.543 g. ) |
| Average orbital speed | 16,758 km / s |
| Inclination ( i ) | 2.546 ° |
| Ascending node longitude (Ω) | 100.549 ° |
| Perihelion Argument (ω) | 57.254 ° |
| Mean Anomaly ( M ) | 339.440 ° |
| physical characteristics | |
| Diameter | 116.69 km |
| Weight | 1.66⋅10 18 kg |
| Density | 2,000 g / cm³ |
| Acceleration of gravity on the surface | 0.0326 m / s² |
| 2nd cosmic speed | 0.0617 km / s |
| Rotation period | 6.665 h |
| Spectral class | C |
| Apparent magnitude | 13.44 m (current) |
| Absolute magnitude | 8.31 m |
| Albedo | 0.0615 |
| Average surface temperature | 159 K (−114 ° C ) |
| Current distance from the Sun | 3.229 a. e. |
| Current distance from Earth | 2.375 a. e. |
Analysis of the light curves obtained in 1979, when the asteroid covered the star Algol , allowed, based on the fluctuation of the star’s brightness, to suggest the presence of a satellite of this asteroid that orbits the main body in a circular orbit with a period of 13.146 hours and the orbit tilted to the line of sight with Earth 15 ° [1] [2] .
Photometric observations conducted in 2006 at the observatory of the Australian city of Leura (Eng.) , Allowed us to obtain the light curves of this body, from which it followed that the period of rotation of the asteroid around its axis is 6.6666 ± 0.0002 hours, with a change in brightness as rotation 0.50 ± 0.02 m [3] .
See also
- List of asteroids ( 101—200 )
- Small Planet Classifications
- Asteroid family
Notes
- ↑ Wijesinghe, MP & Tedesco, EF (December 1979), A test of plausibility of eclipsing binary asteroids , vol. 40, s. 383–393 , DOI 10.1016 / 0019-1035 (79) 90031-9
- ↑ Tedesco, EF Binary asteroids - Evidence for their existence from lightcurves (eng.) // Science: journal. - 1979. - Vol. 203 . - P. 905-907 .
- Ey Oey, Julian (December 2006), Lightcurves analysis of 10 asteroids from the Leura Observatory , vol. 33, p. 96–99