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806 Gyldénia

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806 Gyldénia
Discovery [1]
Discovered byM. F. Wolf
Discovery siteHeidelberg Obs.
Discovery date18 April 1915
Designations
(806) Gyldénia
Named after
Hugo Gyldén
(astronomer)[2]
1915 WX · 1950 LT
main-belt · (outer) [1]
Orbital characteristics [1]
Epoch 16 February 2017 (JD 2457800.5)
Uncertainty parameter 0
Observation arc101.57 yr (37,097 days)
Aphelion3.4506 AU
Perihelion2.9678 AU
3.2092 AU
Eccentricity0.0752
5.75 yr (2,100 days)
280.53°
0° 10m 17.04s / day
Inclination14.240°
43.987°
119.50°
Physical characteristics
Dimensions62.63±1.3 km (IRAS:14)[3]
62.78 km (derived)[4]
67.79±0.89 km[5]
83.10±0.74 km[6]
14.45±0.05 h[7]
14.452±0.001 h[7]
16.846±0.007 h[8]
16.852±0.006 h[9]
16.8537±0.0094 h[10]
0.022±0.001[5]
0.023±0.004[6]
0.0259±0.001 (IRAS:14)[3]
0.0373 (derived)[4]
C [4]
9.953±0.002 (R)[10] · 10.10[6] · 10.2[1][4] · 10.55±0.22[11] · 10.6[3][5]

806 Gyldénia, provisional designation 1915 WX, is a carbonaceous asteroid from the outer region of the asteroid belt, approximately 63 kilometers in diameter. It was discovered on 18 April 1915, by German astronomer Max Wolf at Heidelberg Observatory in southern Germany.[12] The discovery observation was ignored for orbital determination, with the first used observation made at Vienna Observatory on 1 May 2015, reducing the asteroid's observation arc by 2 weeks.[12]

The dark C-type asteroid orbits the Sun at a distance of 3.0–3.5 AU once every 5 years and 9 months (2,100 days). Its orbit has an eccentricity of 0.08 and an inclination of 14° with respect to the ecliptic.[1] Several photometric light-curve analysis rendered a rotation period of 16.852±0.006 hours (best result) with a brightness variation of 0.18 in magnitude (U=3).[9]

According to the surveys carried out by the Infrared Astronomical Satellite, IRAS, the Japanese Akari satellite, and NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, the asteroid's surface has a notably low albedo of less than 0.03, while the Collaborative Asteroid Lightcurve Link derived a somewhat higher value of 0.04.[3][5][6][4]

The minor planet was named in honor of the Fenno-Swedish astronomer Hugo Gyldén (1841–1896), who was a director of the Stockholm Observatory. He developed a new technique to calculate the perturbations of planets and comets. The lunar crater Gyldén is also named after the astronomer (H 80)[2]

References

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  1. ^ a b c d e "JPL Small-Body Database Browser: 806 Gyldenia (1915 WX)" (2016-11-10 last obs.). Jet Propulsion Laboratory. Retrieved 12 December 2016.
  2. ^ a b Schmadel, Lutz D. (2007). "(806) Gyldénia". Dictionary of Minor Planet Names – (806) Gyldénia. Springer Berlin Heidelberg. p. 75. doi:10.1007/978-3-540-29925-7_807. ISBN 978-3-540-00238-3.
  3. ^ a b c d Tedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (October 2004). "IRAS Minor Planet Survey V6.0". NASA Planetary Data System. 12: IRAS-A-FPA-3-RDR-IMPS-V6.0. Bibcode:2004PDSS...12.....T. Retrieved 22 October 2019.
  4. ^ a b c d e "LCDB Data for (806) Gyldenia". Asteroid Lightcurve Database (LCDB). Retrieved 4 July 2016.
  5. ^ a b c d Usui, Fumihiko; Kuroda, Daisuke; Müller, Thomas G.; Hasegawa, Sunao; Ishiguro, Masateru; Ootsubo, Takafumi; et al. (October 2011). "Asteroid Catalog Using Akari: AKARI/IRC Mid-Infrared Asteroid Survey". Publications of the Astronomical Society of Japan. 63 (5): 1117–1138. Bibcode:2011PASJ...63.1117U. doi:10.1093/pasj/63.5.1117. (online, AcuA catalog p. 153)
  6. ^ a b c d Masiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Nugent, C.; et al. (November 2012). "Preliminary Analysis of WISE/NEOWISE 3-Band Cryogenic and Post-cryogenic Observations of Main Belt Asteroids". The Astrophysical Journal Letters. 759 (1): 5. arXiv:1209.5794. Bibcode:2012ApJ...759L...8M. doi:10.1088/2041-8205/759/1/L8. Retrieved 4 July 2016.
  7. ^ a b Behrend, Raoul. "Asteroids and comets rotation curves – (806) Gyldenia". Geneva Observatory. Retrieved 4 July 2016.
  8. ^ Alkema, Michael S. (October 2013). "Asteroid Lightcurve Analysis at Elephant Head Observatory: 2013 April-July". The Minor Planet Bulletin. 40 (4): 215–216. Bibcode:2013MPBu...40..215A. ISSN 1052-8091. Retrieved 1 February 2016.
  9. ^ a b Marciniak, A.; Pilcher, F.; Oszkiewicz, D.; Santana-Ros, T.; Urakawa, S.; Fauvaud, S.; et al. (December 2015). "Against the biases in spins and shapes of asteroids". Planetary and Space Science. 118: 256–266. arXiv:1711.02429. Bibcode:2015P&SS..118..256M. doi:10.1016/j.pss.2015.06.002. Retrieved 4 July 2016.
  10. ^ a b Waszczak, Adam; Chang, Chan-Kao; Ofek, Eran O.; Laher, Russ; Masci, Frank; Levitan, David; et al. (September 2015). "Asteroid Light Curves from the Palomar Transient Factory Survey: Rotation Periods and Phase Functions from Sparse Photometry". The Astronomical Journal. 150 (3): 35. arXiv:1504.04041. Bibcode:2015AJ....150...75W. doi:10.1088/0004-6256/150/3/75. Retrieved 4 July 2016.
  11. ^ Veres, Peter; Jedicke, Robert; Fitzsimmons, Alan; Denneau, Larry; Granvik, Mikael; Bolin, Bryce; et al. (November 2015). "Absolute magnitudes and slope parameters for 250,000 asteroids observed by Pan-STARRS PS1 - Preliminary results". Icarus. 261: 34–47. arXiv:1506.00762. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. Retrieved 4 July 2016.
  12. ^ a b "806 Gyldenia (1915 WX)". Minor Planet Center. Retrieved 4 July 2016.
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