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Davida (minor planet designation: 511 Davida) is a large C-type asteroid. It is the one of the largest asteroids; approximately tied for 7th place, to within measurement uncertainties, and the 5th or 6th most massive. It was discovered by R. S. Dugan in 1903. Davida is named after David Peck Todd, an astronomy professor at Amherst College.

511 Davida
Discovery
Discovered byR. S. Dugan
Discovery dateMay 30, 1903
Designations
Designation
(511) Davida
Pronunciation/dəˈvɪdə, dəˈviːdə/,[1] Latin Dāvīda
Named after
David Peck Todd
Alternative names
1903 LU
Minor planet category
main-belt · (outer)
Meliboea [2]
AdjectivesDavidian /dəˈvɪdiən/[3]
Orbital characteristics[4]
Epoch July 01, 2021
(JD 2459396.5, heliocentric)
Aphelion3.759 AU
Perihelion2.569 AU
Semi-major axis
3.163 AU
Eccentricity0.188
Orbital period (sidereal)
5.626 yr (2055 d)
Mean anomaly
113°
Inclination15.94°
Longitude of ascending node
107.6°
Argument of perihelion
337.2°
Physical characteristics
Dimensionsc/a = 0.70±0.06[5]
(357 ± 2)×(294 ± 2)×(231 ± 50) km[6][7]
Mean diameter
298±4 km[5]
Mass(26.6±7.3)×1018 kg[5]
(38±2)×1018 kg[lower-alpha 1][7]
Mean density
1.92±0.53 g/cm3[5]
2.97±1.30 g/cm3[7]
Synodic rotation period
0.2137 d (5.130 h)
Albedo0.076±0.007 geometric (0.717±0.013 BV, 0.363±0.020)[4]
Temperature~160 K
Spectral type
C
Apparent magnitude
9.50[8] to 12.98
Absolute magnitude (H)
6.43[4]

    Physical characteristics


    Asteroid 511 Davida (lower left at mag 12.5) near galaxy NGC 5792
    Asteroid 511 Davida (lower left at mag 12.5) near galaxy NGC 5792
    3D model of Davida based on lightcurve modeling
    3D model of Davida based on lightcurve modeling
    Keck telescope image sequence of Davida showing its rotation
    Keck telescope image sequence of Davida showing its rotation

    Davida is approximately 270–310 km in diameter and comprises an estimated 1.5% of the total mass of the asteroid belt.[9][10][11] It is a C-type asteroid, which means that it is dark in colouring with a carbonaceous chondrite composition.

    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."


    Mass


    In 2001, Michalak estimated Davida to have a mass of (6.64±0.56)×1019 kg.[12][13] In 2007, Baer and Chesley estimated Davida to have a mass of (5.9±0.6)×1019 kg.[14] As of 2010, Baer suggests Davida has a mass of (3.84±0.20)×1019 kg.[9] This most recent estimate by Baer indicates that Davida is approximately tied with 704 Interamnia as the fifth-most-massive asteroid, though the error bars of Interamnia are large.[9]


    Occultations


    There have been 9 occultation events observed since 1987, many of which produced two or three chords.[15] Two examples shown here.

    Occultations by 511 Davida: Left: Double chord occultation of TYC 5597-01223 on 5 August 2016, observed by two amateur astronomers in eastern Australia. Both observers noted step events, thereby detecting the star has two components. Right: Triple chord occultation of TYC 1964-00787, observed on 6 February 2009 by three astronomers in eastern United States.
    511 Davida occulted TYC 5597-01223 on 5 August 2016. Two observers recorded the event and both observed step events. Shown here is the step recording by Dave Herald.
    511 Davida occulted TYC 5597-01223 on 5 August 2016. Two observers recorded the event and both observed step events. Shown here is the step recording by Dave Herald.

    Notes


    1. (18.96 ± 0.99) × 10−12 M☉

    References


    1. John Daintith & William Gould, eds. (2006) The Facts On File Dictionary of Astronomy. 5th edition. Infobase Publishing.
    2. "Asteroid 511 Davida – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved October 24, 2019.
    3. "Davidian". Merriam-Webster Dictionary.
    4. JPL data Retrieved 2021-09-29
    5. P. Vernazza et al. (2021) VLT/SPHERE imaging survey of the largest main-belt asteroids: Final results and synthesis. Astronomy & Astrophysics 54, A56
    6. 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).
    7. James Baer, Steven Chesley & Robert Matson (2011) "Astrometric masses of 26 asteroids and observations on asteroid porosity." The Astronomical Journal, Volume 141, Number 5
    8. "Bright Minor Planets 2003". Minor Planet Center. Retrieved May 21, 2008.[permanent dead link]
    9. Baer, James (2010). "Recent Asteroid Mass Determinations". Personal Website. Archived from the original on July 2, 2013. Retrieved February 13, 2011.
    10. Pitjeva, E. V. (2005). "High-Precision Ephemerides of Planets—EPM and Determination of Some Astronomical Constants" (PDF). Solar System Research. 39 (3): 176. Bibcode:2005SoSyR..39..176P. doi:10.1007/s11208-005-0033-2. Archived from the original (PDF) on October 31, 2008.
    11. "Baer Mass of 511 Davida" 0.220 / "Mass of Mbelt" 15 = 0.0146
    12. 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. Bibcode:2001A&A...374..703M. doi:10.1051/0004-6361:20010731. Archived from the original on December 4, 2012. Retrieved November 4, 2008.
    13. (3.34±0.28)×10−11 solar masses, per Michalak (2001), extended dynamic model.
    14. Baer, James; Steven R. Chesley (2007). "Astrometric masses of 21 asteroids, and an integrated asteroid ephemeris". Celestial Mechanics and Dynamical Astronomy. Springer Science+Business Media B.V. 2007. 100 (2008): 27–42. Bibcode:2008CeMDA.100...27B. doi:10.1007/s10569-007-9103-8. (2.98±0.30)×10−11 solar masses
    15. "PDS Asteroid/Dust Subnode". sbn.psi.edu. Archived from the original on April 25, 2018. Retrieved April 27, 2018.


    Wikimedia Commons has media related to 511 Davida.


    На других языках

    [de] (511) Davida

    (511) Davida ist ein Asteroid des äußeren Asteroiden-Hauptgürtels, der am 30. Mai 1903 von Raymond Smith Dugan entdeckt wurde. Der Asteroid ist nach dem US-amerikanischen Astronomen David Peck Todd benannt.
    - [en] 511 Davida

    [es] (511) Davida

    (511) Davida es un asteroide perteneciente al cinturón de asteroides descubierto el 30 de mayo de 1903 por Raymond Smith Dugan desde el observatorio de Heidelberg-Königstuhl, Alemania. Está nombrado en honor de David Peck Todd, un profesor de astronomía en el Amherst College.[2]

    [ru] (511) Давида

    (511) Давида (англ. Davida) — астероид главного пояса, принадлежащий к тёмному спектральному классу C. Он был открыт 30 марта 1903 года американским астрономом Раймондом Дуганом и назван в честь Дэвида Тодда[en], профессора астрономии массачусетского колледжа Амхерст. Имя было изменено, так как в то время ещё действовала традиция, согласно которой астероидам давали только женские имена[4].


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