2483 Guinevere

2483 Guinevere
Discovery [1]
Discovered by M. F. Wolf
Discovery site Heidelberg Obs.
Discovery date 17 August 1928
Designations
MPC designation (2483) Guinevere
Pronunciation /ˈɡwɪnᵻvɪər/
Named after
 Guinevere
(Arthurian legend)[2]
1928 QB · 1929 VR
1955 FZ1 · 1961 VM
1961 XR · 1971 BM
1971 FN · 1977 XL
A921 WF
main-belt · (outer) [1]
Hilda [3][4][5]
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 88.51 yr (32,327 days)
Aphelion 5.0733 AU
Perihelion 2.8687 AU
3.9710 AU
Eccentricity 0.2776
7.91 yr (2,890 days)
4.7663°
0° 7m 28.56s / day
Inclination 4.5000°
252.04°
183.36°
Jupiter MOID 0.2309 AU
Physical characteristics
Dimensions 35.687±0.180 km[6]
42.42±2.89 km[7]
44.14 km (derived)[5]
44.17±3.9 km[8]
14.730±0.002 h[9][lower-alpha 1]
14.73081±0.00001 h[10]
14.733 h[11]
0.0396 (derived)[5]
0.0433±0.009[8]
0.048±0.007[7]
0.067±0.011[6]
C [5]
10.60±0.38[12] · 10.8[7][8] · 10.9[1][5]

    2483 Guinevere (/ˈɡwɪnᵻvɪər/), provisional designation 1928 QB, is a dark and elongated Hildian asteroid from the outermost regions of the asteroid belt, approximately 43 kilometers in diameter.

    The asteroid was discovered on 17 August 1928, by German astronomer Max Wolf at Heidelberg Observatory in southwest Germany.[3] In the 1980s, it was named after King Arthur's wife Guinevere.[2]

    Classification and orbit

    Hildian asteroid

    Located in the outermost part of the main-belt, Guinevere is a member of the Hilda family, a large group of asteroids that are thought to have originated from the Kuiper belt. They orbit in a 3:2 orbital resonance with the gas giant Jupiter, meaning that for every 2 orbits Jupiter completes around the Sun, a Hildian asteroid will complete 3 orbits.

    Based on a numerical integration, Guinevere is the Hilda asteroid with the greatest chance of impacting with another asteroid.[4] About 74% of the impact risk occurs when Guinevere is relatively close to perihelion and approaches the main-belt asteroids.

    Orbit

    Guinevere orbits the Sun at a distance of 2.9–5.1 AU once every 7 years and 11 months (2,890 days). Its orbit has an eccentricity of 0.28 and an inclination of 5° with respect to the ecliptic.[1] In November 1921, it was first identified as A921 WF at Bergedorf Observatory in Hamburg, Germany. The body's observation arc begins two nights after its official discovery observation at Heidelberg in August 1928.[3]

    Physical characteristics

    Lightcurves

    During a survey of Hilda asteroids in the 1990s, a rotational lightcurve of Guinevere was obtained from photometric observations by an international collaboration of Swedish, German and Italian astronomers. Lightcurve analysis gave a well-defined rotation period of 14.733 hours with a brightness variation of 1.38 magnitude (U=3).[11]

    Guinevere is a high-amplitude Hilda. A high brightness amplitude typically indicates that the body is elongated and has a non-spheroidal shape. Thermal emission measurements from the Wide-field Infrared Survey Explorer (WISE) gave an even higher amplitude of 1.53 magnitude.[13]:15,24

    In October 2016, another lightcurve of Guinevere was obtained at the Center for Solar System Studies (CS3), Landers, in the Southern California desert, during a photometric survey conducted by American astronomers Dan Coley, Robert Stephens and Brian Warner (U80–U82). It showed a period of 14.730 hours with an amplitude of 0.89 magnitude (U=3-).[9][lower-alpha 1]

    A 2016-published lightcurve, using modeled photometric data from the Lowell Photometric Database (LPD), gave a concurring period of 14.73081 hours (U=n.a.), as well as two spin axis of (19.0°, 70.0°) and (194.0°, 59.0°) in ecliptic coordinates (λ, β).[10]

    Diameter and albedo

    According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and the NEOWISE mission of NASA's WISE spacecraft, Guinevere measures between 35.687 and 44.17 kilometers in diameter and its surface has an albedo between 0.0433 and 0.067.[6][7][8] The Collaborative Asteroid Lightcurve Link agrees with IRAS and derives an albedo of 0.0396 and a diameter of 44.14 kilometers based on an absolute magnitude of 10.9.[5]

    Naming

    This minor planet was named after Guinevere, the wife of King Arthur and the lover of Lancelot in Arthurian legend, after whom the minor planets (2041) and (2597) are named. This affair lead to civil war between King Arthur and his chief knight, who rescued Guinevere from burning at the stake, and initiated the downfall of Arthur's idyllic kingdom.[2]

    The name was suggested by F. Pilcher and the proposal was submitted by Edward Bowell, who also made the object's key identification.[2] The approved naming citation was published by the Minor Planet Center on 24 July 1983, (M.P.C. 8064).[14]

    Notes

    1. 1 2 Lightcurve plot of (2483) Guinevere by B.D. Warner, CS-Palmer Divide Station (October 2016), with a rotation period of 14.730±0.002 hours and a brightness amplitude of 0.089 mag (Quality Code: 3-). Summary figures at Collaborative Asteroid Lightcurve Link (CALL)

    References

    1. 1 2 3 4 5 "JPL Small-Body Database Browser: 2483 Guinevere (1928 QB)" (2017-02-20 last obs.). Jet Propulsion Laboratory. Retrieved 7 July 2017.
    2. 1 2 3 4 Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (2483) Guinevere. Springer Berlin Heidelberg. p. 202. ISBN 978-3-540-00238-3. Retrieved 7 July 2017.
    3. 1 2 3 "2483 Guinevere (1928 QB)". Minor Planet Center. Retrieved 7 July 2017.
    4. 1 2 Dahlgren, M. (August 1998). "A study of Hilda asteroids. III. Collision velocities and collision frequencies of Hilda asteroids". Astronomy and Astrophysics: 1056–1064. Bibcode:1998A&A...336.1056D. Retrieved 7 July 2017.
    5. 1 2 3 4 5 6 "LCDB Data for (2483) Guinevere". Asteroid Lightcurve Database (LCDB). Retrieved 7 July 2017.
    6. 1 2 3 Grav, T.; Mainzer, A. K.; Bauer, J.; Masiero, J.; Spahr, T.; McMillan, R. S.; et al. (January 2012). "WISE/NEOWISE Observations of the Hilda Population: Preliminary Results". The Astrophysical Journal. 744 (2): 15. Bibcode:2012ApJ...744..197G. doi:10.1088/0004-637X/744/2/197. Retrieved 7 July 2017.
    7. 1 2 3 4 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" (PDF). Publications of the Astronomical Society of Japan. 63 (5): 1117–1138. Bibcode:2011PASJ...63.1117U. doi:10.1093/pasj/63.5.1117. Retrieved 7 July 2017.
    8. 1 2 3 4 Tedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (October 2004). "IRAS Minor Planet Survey V6.0". NASA Planetary Data System. Bibcode:2004PDSS...12.....T. Retrieved 7 July 2017.
    9. 1 2 Warner, Brian D.; Stephens, Robert D.; Coley, Daniel R. (April 2017). "Lightcurve Analysis of Hilda Asteroids at the Center for Solar System Studies: 2016 September-December". The Minor Planet Bulletin. 44 (2): 130–137. Bibcode:2017MPBu...44..130W. ISSN 1052-8091. Retrieved 7 July 2017.
    10. 1 2 Durech, J.; Hanus, J.; Oszkiewicz, D.; Vanco, R. (March 2016). "Asteroid models from the Lowell photometric database". Astronomy and Astrophysics. 587: 6. Bibcode:2016A&A...587A..48D. arXiv:1601.02909 Freely accessible. doi:10.1051/0004-6361/201527573. Retrieved 7 July 2017.
    11. 1 2 Dahlgren, M.; Lahulla, J. F.; Lagerkvist, C.-I.; Lagerros, J.; Mottola, S.; Erikson, A.; et al. (June 1998). "A Study of Hilda Asteroids. V. Lightcurves of 47 Hilda Asteroids". Icarus. 133 (2): 247–285. Bibcode:1998Icar..133..247D. doi:10.1006/icar.1998.5919. Retrieved 7 July 2017.
    12. ↑ 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. Bibcode:2015Icar..261...34V. arXiv:1506.00762 Freely accessible. doi:10.1016/j.icarus.2015.08.007. Retrieved 7 July 2017.
    13. ↑ Sonnett, S.; Mainzer, A.; Grav, T.; Masiero, J.; Bauer, J. (February 2015). "Binary Candidates in the Jovian Trojan and Hilda Populations from NEOWISE Light Curves" (PDF). The Astrophysical Journal. 799 (2): 20. Bibcode:2015ApJ...799..191S. arXiv:1412.1853 Freely accessible. doi:10.1088/0004-637X/799/2/191. Retrieved 7 July 2017.
    14. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 7 July 2017.
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