762 Pulcova
|
762 Pulcova and satellite as seen with adaptive optics in 2000[1] | |
| Discovery[2] | |
|---|---|
| Discovered by | G. N. Neujmin |
| Discovery date | 3 September 1913 |
| Designations | |
| 1913 SQ | |
| Main belt | |
| Orbital characteristics[2] | |
| Epoch 31 July 2016 (JD 2457600.5) | |
| Uncertainty parameter 0 | |
| Observation arc | 100.08 yr (36553 d) |
| Aphelion | 3.4801 AU (520.62 Gm) (Q) |
| Perihelion | 2.8291 AU (423.23 Gm) (q) |
| 3.1546 AU (471.92 Gm) (a) | |
| Eccentricity | 0.10319 (e) |
| 5.60 yr (2046.5 d) | |
| 348.62° (M) | |
| 0° 10m 33.276s / day (n) | |
| Inclination | 13.089° (i) |
| 305.76° (Ω) | |
| 189.54° (ω) | |
| Known satellites | S/2000 (762) 1[1] |
| Earth MOID | 1.84297 AU (275.704 Gm) |
| Jupiter MOID | 1.60162 AU (239.599 Gm) |
| Jupiter Tisserand parameter | 3.158 |
| Physical characteristics | |
Mean radius | 68.54±1.6 km |
| Mass | 1.40×1018 kg[3] |
Mean density | 0.90 g/cm3[3] |
| 5.839 h (0.2433 d) | |
Sidereal rotation period | 5.839 hr[2] |
| 0.0458±0.002[2] | |
| 11.93 to 14.79[4] | |
| 8.28[2] | |
|
| |
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 trinary asteroid 45 Eugenia, and binary 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 2 3 "762 Pulcova". SwRI. 2000-02-22. Retrieved 2009-10-20. (AO image)
- 1 2 3 4 5 6 7 "JPL Small-Body Database Browser: 762 Pulcova (1913 SQ)" (2009-09-22 last obs). Retrieved 5 May 2016.
- 1 2 3 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", The Minor Planet Bulletin, 33 (4), pp. 96–99, Bibcode:2006MPBu...33...96O.
- ↑ Dr. William J. Merline & Maria Martinez (2000-10-26). "Astronomers Image Double Asteroid". SwRI Press Release. Retrieved 2009-10-20. (mentions both 90 Antiope and 762 Pulcova)
- 1 2 3 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; et al. (2000-06-21). "Discovery of Companions to Asteroids 762 Pulcova and 90 Antiope by Direct Imaging" (PDF). 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
- 762 Pulcova at the JPL Small-Body Database
