511 Davida
Lua error in Module:Infobox at line 314: malformed pattern (missing ']'). 511 Davida is a large C-type asteroid in the asteroid belt. It was discovered by R. S. Dugan in 1903. It is one of the ten most-massive asteroids, and the 7th-largest asteroid. It is approximately 270–310 km in diameter and comprises an estimated 1.5% of the total mass of the asteroid belt.[5][7][8] It is a C-type asteroid, which means that it is dark in colouring with a carbonaceous chondrite composition.
Davida is one of the few main-belt asteroids whose shape has been determined by ground-based visual observation. From 2002 to 2007, astronomers at the Keck Observatory used the Keck II telescope, which is fitted with adaptive optics, to photograph Davida. The asteroid is not a dwarf planet: there are at least two promontories and at least one flat facet with 15-km deviations from a best-fit ellipsoid. The facet is presumably a 150-km global-scale crater like the ones seen on 253 Mathilde. Conrad et al. (2007) show that craters of this size "can be expected from the impactor size distribution, without likelihood of catastrophic disruption of Davida."
Davida is named after David Peck Todd, an astronomy professor at Amherst College.
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Mass
In 2001, Michalak estimated Davida to have a mass of (6.64±0.56)×1019 kg[9][10] In 2007, Baer and Chesley estimated Davida to have a mass of (5.9±0.6)×1019 kg.[11] As of 2010[update], Baer suggests Davida has a mass of (3.84±0.20)×1019 kg.[5] This most recent estimate by Baer suggests that Davida is less massive than 704 Interamnia, making Davida the sixth-most-massive asteroid, though the error bars overlap.[5]
Occultations
Davida occulted a magnitude-13.3 star on July 14, 2011.[12] Davida occulted the star TYC 0079-00234-1 on August 5, 2013.[13] The event was visible over Argentina and Chile, with Davida at magnitude 11.7 and the star at mag 9.4.[13]
References
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<references />, or <references group="..." />- A.R. Conrad et al. (2007). "Direct measurement of the size, shape, and pole of 511 Davida with Keck AO in a single night", Icarus, doi:10.1016/j.icarus.2007.05.004
External links
- Time lapse photography of Davida
- Al Conrad's research page at Keck
- Orbital simulation from JPL (Java) / Horizons Ephemeris
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- ↑ from Latin Dāvīda
- ↑ də-VY-də or DAV-i-də
- ↑ JPL data Retrieved 2011-09-02
- ↑ Conrad (2007). Measurements of the short axis are less precise than the other two, but also involve a discrepancy between fitting the convolved and deconvolved images (241±40 km), and fitting the edges (191±114 km).
- ↑ 5.0 5.1 5.2 5.3 5.4 Lua error in package.lua at line 80: module 'strict' not found.
- ↑ Lua error in package.lua at line 80: module 'strict' not found.
- ↑ Lua error in package.lua at line 80: module 'strict' not found.
- ↑ "Baer Mass of 511 Davida" 0.220 / "Mass of Mbelt" 15 = 0.0146
- ↑ Lua error in package.lua at line 80: module 'strict' not found.
- ↑ (3.34±0.28)×10−11 solar masses, per Michalak (2001), extended dynamic model.
- ↑ Lua error in package.lua at line 80: module 'strict' not found.
- ↑ Lua error in package.lua at line 80: module 'strict' not found. (chords)
- ↑ 13.0 13.1 Asteroid Occultations
