Astronomy:1551 Argelander

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1551 Argelander
001551-asteroid shape model (1551) Argelander.png
Shape model of Argelander from its lightcurve
Discovery[1]
Discovered byY. Väisälä
Discovery siteTurku Obs.
Discovery date24 February 1938
Designations
(1551) Argelander
Named afterFriedrich Argelander[2]
(German astronomer)
1938 DC1 · 1930 BL
1940 XD · 1951 XG1
1953 GD1 · 1957 KR
1962 XP
Minor planet categorymain-belt[1][3] · (inner)
background[4][5]
Orbital characteristics[3]
Epoch 27 April 2019 (JD 2458600.5)
Uncertainty parameter 0
Observation arc88.76 yr (32,418 d)
|{{{apsis}}}|helion}}2.5539 AU
|{{{apsis}}}|helion}}2.2350 AU
2.3944 AU
Eccentricity0.0666
Orbital period3.71 yr (1,353 d)
Mean anomaly147.41°
Mean motion0° 15m 57.6s / day
Inclination3.7615°
Longitude of ascending node107.23°
233.60°
Physical characteristics
Mean diameter9.19±0.27 km[6]
10.238±0.122 km[7][8]
10.50±0.50 km[9]
11.016±0.073 km[10]
Rotation period4.063±0.006 h[11]
Geometric albedo0.1940[10]
0.217[9]
0.222[7][8]
0.302[6]
S (assumed)[12]
Absolute magnitude (H)12.10[6]
12.20[1][3][7][9][10]


1551 Argelander, provisional designation 1938 DC1, is a background asteroid from the inner regions of the asteroid belt, approximately 10 kilometers (6.2 miles) in diameter. It was discovered on 24 February 1938, by Finnish astronomer Yrjö Väisälä at the Turku Observatory in southwest Finland.[1] The likely S-type asteroid has a rotation period of 4.1 hours.[12] It was named after German astronomer Friedrich Argelander.[2]

Orbit and classification

Argelander is a non-family asteroid from the main belt's background population.[4][5] It orbits the Sun in the inner main-belt at a distance of 2.2–2.6 AU once every 3 years and 9 months (1,353 days; semi-major axis of 2.39 AU). Its orbit has an eccentricity of 0.07 and an inclination of 4° with respect to the ecliptic.[3] The body's observation arc begins with its first observation as 1930 BL at Heidelberg Observatory in January 1930, or 8 years prior to its official discovery observation at Turku.[1]

Naming

This minor planet was named after Friedrich Wilhelm Argelander (1799–1875), author of the famous Bonner Durchmusterung and 19th-century head of the ancient observatory at Turku and Bonn (520).[2] The official naming citation was published by the Minor Planet Center on 30 January 1964 (M.P.C. 2278).[13] The lunar crater Argelander is also named after him.[2]

Physical characteristics

Argelander is an assumed S-type asteroid.[12]

Rotation period and poles

In August 2017, a rotational lightcurve of Argelander was obtained from photometric observations at the Chilean Cerro Tololo Inter-American Observatory using the SARA South Telescope. Lightcurve analysis gave a rotation period of 4.063±0.006 hours and a brightness variation of 0.48 magnitude ({{{1}}}).[11] In January 2012, astronomers at the Palomar Transient Factory had also determined a period of 4.061±0.0023 with an amplitude of 0.41 magnitude ({{{1}}}).[14]

A modeled lightcurve using photometric data from the Lowell Photometric Database was published in 2016. It gave a concurring period of 4.058350±0.000001 hours, as well as two spin axes at (3.0°, −81.0°) and (183.0°, −72.0°) in ecliptic coordinates (λ, β).[15]

Diameter and albedo

According to the surveys carried out by the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Argelander measures between 9.2 and 11.0 kilometers in diameter and its surface has an albedo between 0.19 and 0.30.[6][7][8][9][10] The Collaborative Asteroid Lightcurve Link assumes a standard albedo for a stony asteroid of 0.20 and calculates a diameter of 9.60 kilometers based on an absolute magnitude of 12.45.[12]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 "1551 Argelander (1938 DC1)". Minor Planet Center. https://www.minorplanetcenter.net/db_search/show_object?object_id=1551. Retrieved 11 December 2018. 
  2. ↑ 2.0 2.1 2.2 2.3 Schmadel, Lutz D. (2007). "(1551) Argelander". Dictionary of Minor Planet Names – (1551) Argelander. Springer Berlin Heidelberg. p. 123. doi:10.1007/978-3-540-29925-7_1552. ISBN 978-3-540-00238-3. 
  3. ↑ 3.0 3.1 3.2 3.3 "JPL Small-Body Database Browser: 1551 Argelander (1938 DC1)". Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2001551. Retrieved 11 December 2018. 
  4. ↑ 4.0 4.1 "Asteroid 1551 Argelander". Small Bodies Data Ferret. https://sbntools.psi.edu/ferret/SimpleSearch/results.action?targetName=1551+Argelander. Retrieved 11 December 2018. 
  5. ↑ 5.0 5.1 "Asteroid (1551) Argelander – Proper elements". AstDyS-2, Asteroids – Dynamic Site. https://newton.spacedys.com/astdys/index.php?n=1551&pc=1.1.6. Retrieved 10 December 2018. 
  6. ↑ 6.0 6.1 6.2 6.3 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. doi:10.1088/2041-8205/759/1/L8. Bibcode: 2012ApJ...759L...8M. 
  7. ↑ 7.0 7.1 7.2 7.3 Mainzer, A. K.; Bauer, J. M.; Cutri, R. M.; Grav, T.; Kramer, E. A.; Masiero, J. R. et al. (June 2016). "NEOWISE Diameters and Albedos V1.0". NASA Planetary Data System: EAR-A-COMPIL-5-NEOWISEDIAM-V1.0. Bibcode: 2016PDSS..247.....M. https://sbnarchive.psi.edu/pds3/non_mission/EAR_A_COMPIL_5_NEOWISEDIAM_V1_0/data/neowise_mainbelt.tab. Retrieved 11 December 2018. 
  8. ↑ 8.0 8.1 8.2 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. 
  9. ↑ 9.0 9.1 9.2 9.3 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)
  10. ↑ 10.0 10.1 10.2 10.3 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.  (catalog)
  11. ↑ 11.0 11.1 Fauerbach, Michael; Brown, Austin (July 2018). "Lightcurve Analysis of Minor Planets 1132 Hollandia, 1184 Gaea 1322 Coppernicius, 1551 Argelander, and 3230 Vampilov". The Minor Planet Bulletin 45 (3): 240–241. ISSN 1052-8091. Bibcode: 2018MPBu...45..240F. 
  12. ↑ 12.0 12.1 12.2 12.3 "LCDB Data for (1551) Argelander". Asteroid Lightcurve Database (LCDB). http://www.minorplanet.info/PHP/generateOneAsteroidInfo.php?AstInfo=1551%7CArgelander. Retrieved 11 December 2018. 
  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://cds.cern.ch/record/1339661. 
  14. ↑ 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. 
  15. ↑ Durech, J.; Hanus, J.; Oszkiewicz, D.; Vanco, R. (March 2016). "Asteroid models from the Lowell photometric database". Astronomy and Astrophysics 587: 6. doi:10.1051/0004-6361/201527573. Bibcode: 2016A&A...587A..48D. 

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