Astronomy:2114 Wallenquist

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2114 Wallenquist
Discovery [1]
Discovered byC.-I. Lagerkvist
Discovery siteMount Stromlo Obs.
Discovery date19 April 1976
Designations
(2114) Wallenquist
Named afterÅke Wallenquist
(Swedish astronomer)[2]
1976 HA · 1930 DG
1942 LD · 1953 GZ
1964 FA · 1970 EO3
1970 EZ2
Minor planet categorymain-belt · Themis [3]
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc63.51 yr (23,198 days)
|{{{apsis}}}|helion}}3.6508 AU
|{{{apsis}}}|helion}}2.7467 AU
3.1987 AU
Eccentricity0.1413
Orbital period5.72 yr (2,090 days)
Mean anomaly91.271°
Mean motion0° 10m 20.28s / day
Inclination0.5558°
Longitude of ascending node1.5530°
216.98°
Physical characteristics
Dimensions21.12±1.26 km[4]
22.558±0.079[5]
23.008±0.190 km[6]
27.45 km (derived)[3]
27.67±2.3 km (IRAS:2)[7]
Rotation period5.49±0.01 h[8]
5.5078±0.0009 h[9]
5.510±0.005 h[10]
Geometric albedo0.0447 (derived)[3]
0.0838±0.016 (IRAS:2)[7]
0.1216±0.0099[6]
0.145±0.019[5]
0.149±0.020[4]
S [3]
Absolute magnitude (H)11.1[7][4][6] · 11.749±0.002 (R)[9] · 11.8[1][3] · 11.87±0.23[11]


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.[12]

Orbit and classification

Wallenquist is a member of the Themis family, a dynamical family of outer-belt asteroids with nearly coplanar ecliptical orbits. It orbits the Sun in the outer main-belt at a distance of 2.7–3.7 AU once every 5 years and 9 months (2,090 days). Its orbit has an eccentricity of 0.14 and an inclination of 1° with respect to 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.[12]

Physical characteristics

Rotation period

In April 2010, a rotational lightcurve of Wallenquist obtained by American astronomer Robert Stephens at the Goat Mountain Astronomical Research Station (GMARS, G79), California, gave a well-defined rotation period of 5.510 hours with a brightness amplitude of 0.22 magnitude ({{{1}}}).[10]

Two other observations, by French astronomer René Roy at Blauvac Observatory (627), 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 ({{{1}}}).[8][9]

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 Wide-field Infrared Survey Explorer, Wallenquist 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][7]

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 characterizes the body as a S-type rather than a darker C-type asteroid.[3]

Naming

This 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.[2]

After his retirement Wallenquist continued to research dark matter in open clusters at the Uppsala Astronomical Observatory. He co-discovered the near-Earth Amor asteroid 1980 Tezcatlipoca during his stay at the Palomar Observatory in California in 1950.[2] The official naming citation was published by the Minor Planet Center on 1 February 1979 (M.P.C. 4645).[13]

References

  1. ↑ 1.0 1.1 1.2 1.3 "JPL Small-Body Database Browser: 2114 Wallenquist (1976 HA)". Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2002114. Retrieved 11 June 2017. 
  2. ↑ 2.0 2.1 2.2 Schmadel, Lutz D. (2007). "(2114) Wallenquist". Dictionary of Minor Planet Names – (2114) Wallenquist. Springer Berlin Heidelberg. pp. 171–172. doi:10.1007/978-3-540-29925-7_2115. ISBN 978-3-540-00238-3. 
  3. ↑ 3.0 3.1 3.2 3.3 3.4 3.5 "LCDB Data for (2114) Wallenquist". Asteroid Lightcurve Database (LCDB). http://www.minorplanet.info/PHP/generateOneAsteroidInfo.php?AstInfo=2114%7CWallenquist. Retrieved 4 July 2016. 
  4. ↑ 4.0 4.1 4.2 4.3 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. doi:10.1093/pasj/63.5.1117. Bibcode: 2011PASJ...63.1117U.  (online, AcuA catalog p. 153)
  5. ↑ 5.0 5.1 5.2 Masiero, Joseph R.; Grav, T.; Mainzer, A. K.; Nugent, C. R.; Bauer, J. M.; Stevenson, R. et al. (August 2014). "Main-belt Asteroids with WISE/NEOWISE: Near-infrared Albedos". The Astrophysical Journal 791 (2): 11. doi:10.1088/0004-637X/791/2/121. Bibcode: 2014ApJ...791..121M. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2014ApJ...791..121M. Retrieved 7 December 2016. 
  6. ↑ 6.0 6.1 6.2 6.3 Mainzer, A.; Grav, T.; Masiero, J.; Hand, E.; Bauer, J.; Tholen, D. et al. (November 2011). "NEOWISE Studies of Spectrophotometrically Classified Asteroids: Preliminary Results". The Astrophysical Journal 741 (2): 25. doi:10.1088/0004-637X/741/2/90. Bibcode: 2011ApJ...741...90M. 
  7. ↑ 7.0 7.1 7.2 7.3 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. https://sbnarchive.psi.edu/pds3/iras/IRAS_A_FPA_3_RDR_IMPS_V6_0/data/diamalb.tab. Retrieved 22 October 2019. 
  8. ↑ 8.0 8.1 Behrend, Raoul. "Asteroids and comets rotation curves – (2114) Wallenquist". Geneva Observatory. http://obswww.unige.ch/~behrend/page4cou.html#002114. Retrieved 4 July 2016. 
  9. ↑ 9.0 9.1 9.2 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. doi:10.1088/0004-6256/150/3/75. Bibcode: 2015AJ....150...75W. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2015AJ....150...75W. Retrieved 4 July 2016. 
  10. ↑ 10.0 10.1 Stephens, Robert D. (October 2010). "Asteroids Observed from GMARS and Santana Observatories: 2010 April - June". The Minor Planet Bulletin 37 (4): 159–161. ISSN 1052-8091. Bibcode: 2010MPBu...37..159S. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2010MPBu...37..159S. 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. doi:10.1016/j.icarus.2015.08.007. Bibcode: 2015Icar..261...34V. http://adsabs.harvard.edu/cgi-bin/bib_query?bibcode=2015Icar..261...34V. Retrieved 4 July 2016. 
  12. ↑ 12.0 12.1 "2114 Wallenquist (1976 HA)". Minor Planet Center. https://www.minorplanetcenter.net/db_search/show_object?object_id=2114. Retrieved 4 July 2016. 
  13. ↑ Schmadel, Lutz D. (2009). "Appendix – Publication Dates of the MPCs". Dictionary of Minor Planet Names – Addendum to Fifth Edition (2006–2008). Springer Berlin Heidelberg. p. 221. doi:10.1007/978-3-642-01965-4. ISBN 978-3-642-01964-7. https://archive.org/details/dictionaryminorp2008schm. 

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