511 Davida: Difference between revisions

From Wikipedia, the free encyclopedia
Browse history interactively
← Previous editNext edit →
Content deleted Content added
VisualWikitext
mNo edit summary
704 Interamnia should easily be more massive. Add Baer2007 Mass of 5.9E+19
Line 20: Line 20:
| dimensions=289±21 km (357±2 × 294±2 × 231±50)<ref>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
| dimensions=289±21 km (357±2 × 294±2 × 231±50)<ref>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&nbsp;km), and fitting the edges (191±114&nbsp;km).</ref>
images (241±40&nbsp;km), and fitting the edges (191±114&nbsp;km).</ref>
| mass= (6.64±0.56)×10<sup>19</sup> [[kilogram|kg]]<ref name=Michalak2001>{{cite journal
| mass=5.9×10<sup>19</sup> [[kilogram|kg]]<ref name="Baer2007">{{cite journal
|last=Baer |first=James
|coauthors=Steven R. Chesley
|title=Astrometric masses of 21 asteroids, and an integrated asteroid ephemeris
|journal=Celestial Mechanics and Dynamical Astronomy
|volume=100 |issue=2008 |pages=27-42
|publisher=Springer Science+Business Media B.V. 2007
|url=http://www.springerlink.com/content/h747307j43863228/fulltext.pdf
|format=[[PDF]]
|doi=10.1007/s10569-007-9103-8
|accessdate=2008-11-15 }}</ref><ref name=DavidaMass2008>(2.98±0.30)×10<sup>−11</sup> * [[sun|1.9891×10<sup>30</sup>]] = 5.9×10<sup>19</sup> kg, per Baer/Chesley (2008).</ref><br>(6.64±0.56)×10<sup>19</sup> kg<ref name=Michalak2001>{{cite journal
|last=Michalak |first=G.
|last=Michalak |first=G.
|title=Determination of asteroid masses (6) Hebe, (10) Hygiea, (15) Eunomia, (52) Europa, (88) Thisbe, (444) Gyptis, (511) Davida and (704) Interamnia
|title=Determination of asteroid masses (6) Hebe, (10) Hygiea, (15) Eunomia, (52) Europa, (88) Thisbe, (444) Gyptis, (511) Davida and (704) Interamnia
Line 28: Line 38:
|url=http://www.aanda.org/index.php?option=article&access=standard&Itemid=129&url=/articles/aa/abs/2001/29/aa10228/aa10228.html
|url=http://www.aanda.org/index.php?option=article&access=standard&Itemid=129&url=/articles/aa/abs/2001/29/aa10228/aa10228.html
|accessdate=2008-11-04 }}</ref><ref>(3.34±0.28)×10<sup>−11</sup> solar masses, per Michalak (2001), extended dynamic model.</ref>
|accessdate=2008-11-04 }}</ref><ref>(3.34±0.28)×10<sup>−11</sup> solar masses, per Michalak (2001), extended dynamic model.</ref>
| density= 5.2±1.6 g/[[cubic centimetre|cm³]]<ref>Calculated from the above figures.</ref>
| density= 5.2±1.6 g/[[cubic centimetre|cm³]]<ref>Calculated from Michalak (2001) figures.</ref>
| rotation= 0.2137235 d (5.13 h)
| rotation= 0.2137235 d (5.13 h)
| spectral_type=C
| spectral_type=C

Revision as of 02:02, 15 November 2008

511 Davida
File:511 davida.jpg
Asteroid 511 Davida imaged by the Keck Observatory, December 2002.
Discovery
Discovered byR. S. Dugan
Discovery dateMay 30, 1903
Designations
1903 LU
Main belt
Orbital characteristics
Epoch October 22, 2004 (JD 2453300.5)
Aphelion561.538 Gm (3.754 AU)
Perihelion385.946 Gm (2.580 AU)
473.742 Gm (3.167 AU)
Eccentricity0.185
2058.370 d (5.64 a)
16.59 km/s
124.997°
Inclination15.936°
107.683°
338.694°
Physical characteristics
Dimensions289±21 km (357±2 × 294±2 × 231±50)[1]
Mass5.9×1019 kg[2][3]
(6.64±0.56)×1019 kg[4][5]
Mean density
5.2±1.6 g/cm³[6]
0.2137235 d (5.13 h)
Albedo0.054–0.066 2
Temperature~160 K
Spectral type
C
9.50[7] to 12.98
6.22

511 Davida (Template:PronEng də-VEE-də) is a large main belt C-type asteroid. It was discovered by R. S. Dugan in 1903. It is thought to be one of the ten most massive asteroids. It is approximately 270–310 km in diameter and comprises an estimated 1% of the total mass of the asteroid belt. It is a C-type asteroid, which means that it is dark in colouring with a carbonate 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.

External links

References

  1. ^ 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).
  2. ^ Baer, James. "Astrometric masses of 21 asteroids, and an integrated asteroid ephemeris" (PDF). Celestial Mechanics and Dynamical Astronomy. 100 (2008). Springer Science+Business Media B.V. 2007: 27–42. doi:10.1007/s10569-007-9103-8. Retrieved 2008-11-15. {{cite journal}}: Unknown parameter |coauthors= ignored (|author= suggested) (help)
  3. ^ (2.98±0.30)×10−11 * 1.9891×1030 = 5.9×1019 kg, per Baer/Chesley (2008).
  4. ^ Michalak, G. (2001). "Determination of asteroid masses (6) Hebe, (10) Hygiea, (15) Eunomia, (52) Europa, (88) Thisbe, (444) Gyptis, (511) Davida and (704) Interamnia". Astronomy & Astrophysics. 374: 703–711. doi:10.1051/0004-6361:20010731. Retrieved 2008-11-04.
  5. ^ (3.34±0.28)×10−11 solar masses, per Michalak (2001), extended dynamic model.
  6. ^ Calculated from Michalak (2001) figures.
  7. ^ "Bright Minor Planets 2003". Minor Planet Center. Retrieved 2008-05-21.
Wikimedia Commons has media related to 511 Davida.
Retrieved from "https://en.wikipedia.org/w/index.php?title=511_Davida&oldid=251887375"