1864 Daedalus

1864 Daedalus
Discovery [1]
Discovered by T. Gehrels
Discovery site Palomar Obs.
Discovery date 24 March 1971
Designations
MPC designation (1864) Daedalus
Pronunciation /ˈdɛdləs/ DED-ləs
Named after
 Daedalus (Greek mythology)[2]
1971 FA
Apollo · NEO [1][3]
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 46.14 yr (16,854 days)
Aphelion 2.3586 AU
Perihelion 0.5634 AU
1.4610 AU
Eccentricity 0.6144
1.77 yr (645 days)
23.049°
0° 33m 29.16s / day
Inclination 22.211°
6.6379°
325.64°
Earth MOID 0.2693 AU
Physical characteristics
Dimensions 2.722±0.114 km[4]
3.00 km (derived)[5]
3.7 km[6]
8.57 h[7]
8.572 h[8]
8.575±0.002 h[9]
0.20 (assumed)[5]
0.273±0.055[4][6]
SQ (Tholen)[1] · Sr (SMASS)[1]
Sq [10] · S [5]
B–V = 0.830[1]
U–B = 0.500[1]
14.85[1][4] · 14.98[5][8]

    1864 Daedalus, provisional designation 1971 FA, is a stony asteroid and near-Earth object of the Apollo group, approximately 3 kilometers in diameter. It was discovered on 24 March 1971, by Dutch–American astronomer Tom Gehrels at Palomar Observatory, California, and named after Daedalus from Greek mythology.[3]

    Orbit and classification

    Daedalus is a member of the Apollo asteroids, a group of near-Earth object with an Earth-crossing orbit. It orbits the Sun in the inner main-belt at a distance of 0.6–2.4 AU once every 1 years and 9 months (645 days). Its orbit has an eccentricity of 0.61 and an inclination of 22° with respect to the ecliptic.[1] It has an Earth Minimum orbit intersection distance (MOID) of 0.2693 AU.[1]

    Physical characteristics

    Daedalus is a stony asteroid, characterized as an SQ and Sr spectral type in the Tholen and SMASS taxonomy.[1]

    Diameter and albedo

    According to the survey carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, it measures 2.7 and 3.7 kilometers in diameter, respectively, and its surface has an albedo of 0.273.[4][6] The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and derives a diameter of 3.0 kilometers based on an absolute magnitude of 14.98.[5]

    Rotation period

    Several rotational lightcurves of Daedalus were obtained by astronomers Tom Gehrels, Petr Pravec and Brian Warner. Lightcurve analysis gave a concurring rotation period of 8.572 hours with a high brightness variation of 0.85–1.04 magnitude, indicating a non-spheroidal shape (U=3/3/3).[7][8][9]

    Naming

    This minor planet was named after the Greek mythological figure Daedalus, the builder of King Minos' labyrinth, who was subsequently imprisoned there with his son Icarus. They escaped on wings of feathers and wax, but whereas Icarus was drowned when the wax in his wings melted, Daedalus went on to Sicily and built there a temple to Apollo. There is also a lunar crater called Daedalus.[2] The official naming citation was published by the Minor Planet Center before November 1977 (M.P.C. 3758).[11]

    References

    1. 1 2 3 4 5 6 7 8 9 10 11 "JPL Small-Body Database Browser: 1864 Daedalus (1971 FA)" (2017-05-15 last obs.). Jet Propulsion Laboratory. Retrieved 9 June 2017.
    2. 1 2 Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (1864) Daedalus. Springer Berlin Heidelberg. p. 149. ISBN 978-3-540-00238-3. Retrieved 12 December 2016.
    3. 1 2 "1864 Daedalus (1971 FA)". Minor Planet Center. Retrieved 12 December 2016.
    4. 1 2 3 4 Mainzer, A.; Grav, T.; Masiero, J.; Hand, E.; Bauer, J.; Tholen, D.; et al. (November 2011). "NEOWISE Studies of Spectrophotometrically Classified Asteroids: Preliminary Results" (PDF). The Astrophysical Journal. 741 (2): 25. Bibcode:2011ApJ...741...90M. arXiv:1109.6407 Freely accessible. doi:10.1088/0004-637X/741/2/90. Retrieved 12 December 2016.
    5. 1 2 3 4 5 "LCDB Data for (1864) Daedalus". Asteroid Lightcurve Database (LCDB). Retrieved 12 December 2016.
    6. 1 2 3 Mainzer, A.; Grav, T.; Bauer, J.; Masiero, J.; McMillan, R. S.; Cutri, R. M.; et al. (December 2011). "NEOWISE Observations of Near-Earth Objects: Preliminary Results". The Astrophysical Journal. 743 (2): 17. Bibcode:2011ApJ...743..156M. arXiv:1109.6400 Freely accessible. doi:10.1088/0004-637X/743/2/156. Retrieved 12 December 2016.
    7. 1 2 Gehrels, T.; Roemer, E.; Marsden, B. G. (September 1971). "Minor Planets and Related Objects. VIL Asteroid 1971 FA". Astronomical Journal. 76: 607. Bibcode:1971AJ.....76..607G. doi:10.1086/111169. Retrieved 12 December 2016.
    8. 1 2 3 Pravec, P.; Wolf, M.; Varady, M.; Bárta, P. (December 1995). "CCD Photometry of 6 Near-Earth Asteroids". Earth. 71 (3): 177–187. Bibcode:1995EM&P...71..177P. doi:10.1007/BF00612955. Retrieved 12 December 2016.
    9. 1 2 Warner, Brian D. (July 2015). "Near-Earth Asteroid Lightcurve Analysis at CS3-Palmer Divide Station: 2015 January - March". The Minor Planet Bulletin. 42 (3): 172–183. Bibcode:2015MPBu...42..172W. ISSN 1052-8091. Retrieved 12 December 2016.
    10. ↑ Thomas, Cristina A.; Emery, Joshua P.; Trilling, David E.; Delbó, Marco; Hora, Joseph L.; Mueller, Michael (January 2014). "Physical characterization of Warm Spitzer-observed near-Earth objects". Icarus. 228: 217–246. Bibcode:2014Icar..228..217T. arXiv:1310.2000 Freely accessible. doi:10.1016/j.icarus.2013.10.004. Retrieved 12 December 2016.
    11. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 12 December 2016.
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