2114 Wallenquist

2114 Wallenquist
Discovery [1]
Discovered by C.-I. Lagerkvist
Discovery site Mount Stromlo Obs.
Discovery date 19 April 1976
Designations
MPC designation 2114 Wallenquist
Named after
 Åke Wallenquist
(astronomer)[2]
1976 HA · 1930 DG
1942 LD · 1953 GZ
1964 FA · 1970 EO3
1970 EZ2
main-belt · Themis [3]
Orbital characteristics [1]
Epoch 31 July 2016 (JD 2457600.5)
Uncertainty parameter 0
Observation arc 63.19 yr (23,080 days)     
Aphelion 3.6502 AU
Perihelion 2.7459 AU
3.1981 AU
Eccentricity 0.1414
5.72 yr (2,089 days)
22.441°
0° 10m 20.28s / day
Inclination 0.5559°
1.5451°
216.88°
Physical characteristics
Dimensions 21.12±1.26 km[4]
23.008±0.190 km[5]
27.45 km (derived)[3]
27.67±2.3 km (IRAS:2)[6]
5.49±0.01 h[7]
5.5078±0.0009 h[8]
5.510±0.005 h[9]
0.0447 (derived)[3]
0.0838±0.016 (IRAS:2)[6]
0.1216±0.0099[5]
0.149±0.020[4]
S [3]
11.1[6][4][5]
11.749±0.002 (R)[8]
11.8[1][3]
11.87±0.23[10]

    2114 Wallenquist, provisional designation 1976 HA, is a Themistian asteroid from the outer region of the asteroid belt, approximately 28 kilometers in diameter. It was discovered by Swedish astronomer Claes-Ingvar Lagerkvist at the Australian Mount Stromlo Observatory near Canberra, on 19 April 1976.[11]

    The asteroid is a member of the Themis family, a dynamical family of outer-belt asteroids with nearly coplanar ecliptical orbits. It orbits the Sun at a distance of 2.7–3.7 AU once every 5 years and 9 months (2,089 days). Its orbit has an eccentricity of 0.14 and an inclination of 1° with respect to the plane of the ecliptic.[1] The first used observation was made at the U.S. Goethe Link Observatory in 1953, extending the asteroid's observation arc by 23 years prior to its discovery.[11]

    In April 2010, a rotational light-curve obtained at the U.S. Goat Mountain Astronomical Research Station (GMARS), California, rendered a well-defined rotation period of 5.510±0.005 hours with a brightness amplitude of 0.22 in magnitude (U=3).[9] Two other observations, by French astronomer René Roy at Blauvac Observatory, France, and by astronomers at the U.S. Palomar Transient Factory gave a period of 5.49±0.01 and 5.5078±0.0009, with an amplitude of 0.30 and 0.23, respectively (U=2/2).[7][8]

    According to the surveys carried out by the Infrared Astronomical Satellite, IRAS, the Japanese Akari satellite, and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, the asteroid measures between 21.1 and 27.6 kilometers in diameter while its surface has an albedo in the range of 0.08 and 0.15.[4][5][6] The Collaborative Asteroid Lightcurve Link (CALL) derives an even lower albedo of 0.04 and calculates a diameter of 27.5 kilometer. Despite its low albedo, CALL classifies the body as a S-type rather than a darker C-type asteroid.[3]

    The minor planet was named in honor of Swedish astronomer Åke Wallenquist (1904–1994), former director of the Kvistaberg Station, after which the minor planet 3331 Kvistaberg is named. After his retirement he continued to research dark matter in open clusters at the Uppsala Astronomical Observatory. Wallenquist co-discovered the near-Earth Amor asteroid 1980 Tezcatlipoca during his stay at the U.S. Palomar Observatory in 1950.[2] Naming citation was published before November 1977 (M.P.C. 4645).[12]

    References

    1. 1 2 3 4 "JPL Small-Body Database Browser: 2114 Wallenquist (1976 HA)" (2016-06-13 last obs.). Jet Propulsion Laboratory. Retrieved 4 July 2016.
    2. 1 2 Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (2114) Wallenquist. Springer Berlin Heidelberg. pp. 171–172. ISBN 978-3-540-00238-3. Retrieved 4 July 2016.
    3. 1 2 3 4 5 6 "LCDB Data for (2114) Wallenquist". Asteroid Lightcurve Database (LCDB). Retrieved 4 July 2016.
    4. 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". Publications of the Astronomical Society of Japan. 63 (5): 1117–1138. Bibcode:2011PASJ...63.1117U. doi:10.1093/pasj/63.5.1117. Retrieved 4 July 2016.
    5. 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. arXiv:1109.6407Freely accessible. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. Retrieved 4 July 2016.
    6. 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 4 July 2016.
    7. 1 2 Behrend, Raoul. "Asteroids and comets rotation curves – (2114) Wallenquist". Geneva Observatory. Retrieved 4 July 2016.
    8. 1 2 3 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:1504.04041Freely accessible. Bibcode:2015AJ....150...75W. doi:10.1088/0004-6256/150/3/75. Retrieved 4 July 2016.
    9. 1 2 Stephens, Robert D. (October 2010). "Asteroids Observed from GMARS and Santana Observatories: 2010 April - June". The Minor Planet Bulletin. 37 (4): 159–161. Bibcode:2010MPBu...37..159S. ISSN 1052-8091. Retrieved 4 July 2016.
    10. ↑ 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:1506.00762Freely accessible. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. Retrieved 4 July 2016.
    11. 1 2 "2114 Wallenquist (1976 HA)". Minor Planet Center. Retrieved 4 July 2016.
    12. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 4 July 2016.

    External links

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