762 Pulcova
 762 Pulcova and satellite as seen with adaptive optics in 2000[1] | |
| Discovery[2] | |
|---|---|
| Discovered by | G. N. Neujmin |
| Discovery date | September 3, 1913 |
| Designations | |
| Alternative names | 1913 SQ |
| Minor planet category | Main belt |
| Orbital characteristics[2] | |
| Epoch January 4, 2010 (2455200.5) | |
| Aphelion | 3.4744 AU (Q) |
| Perihelion | 2.8343 AU (q) |
| Semi-major axis | 3.1543 AU (a) |
| Eccentricity | 0.10146 |
| Orbital period | 5.60 yr |
| Mean anomaly | 287.18° (M) |
| Inclination | 13.089° |
| Longitude of ascending node | 305.79° |
| Argument of perihelion | 189.06° |
| Known satellites | S/2000 (762) 1[1] |
| Physical characteristics | |
| Dimensions | 137.08 km[2] |
| Mass | 1.40×1018 kg[3] |
| Mean density | 0.90 g/cm3[3] |
| Sidereal rotation period | 5.839 hr[2] |
| Albedo | 0.0458[2] |
| Apparent magnitude | 11.93 to 14.79[4] |
| Absolute magnitude (H) | 8.28[2] |
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762 Pulcova is a main-belt asteroid. It was discovered by Grigoriy N. Neujmin in 1913,[2] and is named after Pulkovo Observatory, near Saint Petersburg. Pulcova is 137 km in diameter,[2] and is a C-type asteroid, which means that it is dark in colouring with a carbonate composition.
Photometric observations of this asteroid from Leura, Australia during 2006 gave a light curve with a period of 5.8403 ± 0.0005 hours and a brightness variation of 0.20 ± 0.02 in magnitude. This result is in agreement with previous studies.[5]
Satellite
On February 22, 2000,[1] astronomers at the Canada-France-Hawaii Telescope on Mauna Kea, Hawaii, discovered a small, 15-km moon (roughly a 10th the size of the primary)[6] orbiting Pulcova at a distance of 800 km.[7] Its orbital period is 4 days.[8] The satellite is about 4 magnitudes fainter than the primary.[7] It was one of the first asteroid moons to be identified.
Density
In the year 2000, Merline estimated Pulcova to have a density of 1.8 g/cm³, which would make it more dense than the binary asteroids 45 Eugenia and 90 Antiope.[7] But estimates by Marchis in 2008 suggest a density of only 0.90 g/cm³,[3] suggesting it may be a loosely-packed rubble pile, not a monolithic object.
References
- ↑ 1.0 1.1 1.2 "762 Pulcova". SwRI. 2000-02-22. Retrieved 2009-10-20. (AO image)
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 "JPL Small-Body Database Browser: 762 Pulcova (1913 SQ)". 2009-09-22 last obs. Retrieved 2009-10-20.
- ↑ 3.0 3.1 3.2 Jim Baer (2008). "Recent Asteroid Mass Determinations". Personal Website. Retrieved 2008-11-28.
- ↑ Magnitudes generated with JPL Horizons for the year 1950 through 2100
- ↑ Oey, Julian (December 2006), "Lightcurves analysis of 10 asteroids from Leura Observatory", Bulletin of the Minor Planets Section of the Association of Lunar and Planetary Observers 33 (4): 96–99, Bibcode:2006MPBu...33...96O.
- ↑ Dr. William J. Merline and Maria Martinez (2000-10-26). "Astronomers Image Double Asteroid". SwRI Press Release. Retrieved 2009-10-20. (mentions both 90 Antiope and 762 Pulcova)
- ↑ 7.0 7.1 7.2 W.J. Merline (SwRI), L.M. Close (ESO, U. Arizona), C. Dumas (JPL), J.C. Shelton (Mt. Wilson Obs.), F. Menard (CFHT), C.R. Chapman, D.C. Slater (SwRI) (2000-06-21). "Discovery of Companions to Asteroids 762 Pulcova and 90 Antiope by Direct Imaging". SwRI. Retrieved 2009-10-21.
- ↑ Johnston, Robert (September 1, 2005). "(762) Pulcova". Johnston's Archive. Retrieved 1 November 2013.
External links
- Orbital simulation from JPL (Java) / Ephemeris
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