762 Pulcova

762 Pulcova
762 Pulcova and satellite as seen with adaptive optics in 2000[1]
Discovery[2]
Discovered byG. N. Neujmin
Discovery date3 September 1913
Designations
(762) Pulcova
Pronunciation/ˈpʊlkəvə/
Named after
Pulkovo Heights
1913 SQ
Main belt
AdjectivesPulcovian /pʊlˈkoʊviən/[3]
Orbital characteristics[2]
Epoch 31 July 2016 (JD 2457600.5)
Uncertainty parameter 0
Observation arc100.08 yr (36553 d)
Aphelion3.4801 AU (520.62 Gm) (Q)
Perihelion2.8291 AU (423.23 Gm) (q)
3.1546 AU (471.92 Gm) (a)
Eccentricity0.10319 (e)
5.60 yr (2046.5 d)
348.62° (M)
0° 10m 33.276s / day (n)
Inclination13.089° (i)
305.76° (Ω)
189.54° (ω)
Known satellitesS/2000 (762) 1[1]
Earth MOID1.84297 AU (275.704 Gm)
Jupiter MOID1.60162 AU (239.599 Gm)
TJupiter3.158
Physical characteristics
68.54±1.6 km
Mass1.40×1018 kg[4]
Mean density
0.90 g/cm3[4]
5.839 h (0.2433 d)
5.839 hr[2]
0.0458±0.002[2]
11.93 to 14.79[5]
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.[6]

Satellite

Pulcova and its satellite imaged by the Hubble Space Telescope in January 2005
Diagram of 762 Pulcova's orbit

On February 22, 2000,[1] astronomers at the Canada-France-Hawaii Telescope on Mauna Kea, Hawaii, discovered a 15-km moon (roughly a tenth the size of the primary)[7] orbiting Pulcova at a distance of 800 km.[8] Its orbital period is 4 days.[9] The satellite is about 4 magnitudes fainter than the primary.[8] 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.[8] But estimates by Marchis in 2008 suggest a density of only 0.90 g/cm3,[4] suggesting it may be a loosely packed rubble pile, not a monolithic object.

References

  1. ^ a b c "762 Pulcova". SwRI. 22 February 2000. Retrieved 20 October 2009. (AO image)
  2. ^ a b c d e f g "JPL Small-Body Database Browser: 762 Pulcova (1913 SQ)" (2009-09-22 last obs). Retrieved 5 May 2016.
  3. ^ Catalogue of the Mathematical, Historical, Bibliographical and Miscellaneous Portion of the Celebrated Library of M. Guglielmo Libri, 1861, p. 216
  4. ^ a b c Jim Baer (2008). "Recent Asteroid Mass Determinations". Personal Website. Archived from the original on 2 July 2013. Retrieved 28 November 2008.
  5. ^ Magnitudes generated with JPL Horizons for the year 1950 through 2100
  6. ^ Oey, Julian (December 2006), "Lightcurves analysis of 10 asteroids from Leura Observatory", The Minor Planet Bulletin, 33 (4): 96–99, Bibcode:2006MPBu...33...96O.
  7. ^ Dr. William J. Merline & Maria Martinez (26 October 2000). "Astronomers Image Double Asteroid". SwRI Press Release. Retrieved 20 October 2009. (mentions both 90 Antiope and 762 Pulcova)
  8. ^ a b c 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. (21 June 2000). "Discovery of Companions to Asteroids 762 Pulcova and 90 Antiope by Direct Imaging" (PDF). SwRI. Retrieved 21 October 2009.
  9. ^ Johnston, Robert (1 September 2005). "(762) Pulcova". Johnston's Archive. Retrieved 1 November 2013.