1551 Argelander

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1551 Argelander
Discovery [1]
Discovered byY. Väisälä
Discovery siteTurku Obs.
Discovery date24 February 1938
MPC designation(1551) Argelander
Named after
Friedrich Argelander[2]
(German astronomer)
1938 DC1 · 1930 BL
1940 XD · 1951 XG1
1953 GD1 · 1957 KR
1962 XP
main-belt[1][3] · (inner)
Orbital characteristics[3]
Epoch 27 April 2019 (JD 2458600.5)
Uncertainty parameter 0
Observation arc88.76 yr (32,418 d)
Aphelion2.5539 AU
Perihelion2.2350 AU
2.3944 AU
3.71 yr (1,353 d)
0° 15m 57.6s / day
Physical characteristics
Mean diameter
9.19±0.27 km[6]
10.238±0.122 km[7][8]
10.50±0.50 km[9]
11.016±0.073 km[10]
4.063±0.006 h[11]
S (assumed)[12]

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[edit]

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]


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 before November 1977 (M.P.C. 2278).[13] The lunar crater Argelander is also named after him.[2]

Physical characteristics[edit]

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

Rotation period and poles[edit]

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 (U=2+).[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 (U=2).[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[edit]

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]


  1. ^ a b c d e "1551 Argelander (1938 DC1)". Minor Planet Center. Retrieved 11 December 2018.
  2. ^ a b c d Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (1551) Argelander. Springer Berlin Heidelberg. p. 123. ISBN 978-3-540-00238-3. Retrieved 11 December 2018.
  3. ^ a b c d "JPL Small-Body Database Browser: 1551 Argelander (1938 DC1)" (2018-10-20 last obs.). Jet Propulsion Laboratory. Retrieved 11 December 2018.
  4. ^ a b "Asteroid 1551 Argelander". Small Bodies Data Ferret. Retrieved 11 December 2018.
  5. ^ a b "Asteroid (1551) Argelander – Proper elements". AstDyS-2, Asteroids – Dynamic Site. Retrieved 10 December 2018.
  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" (PDF). The Astrophysical Journal Letters. 759 (1): 5. arXiv:1209.5794. Bibcode:2012ApJ...759L...8M. doi:10.1088/2041-8205/759/1/L8. Retrieved 11 December 2018.
  7. ^ a b c d 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. Bibcode:2016PDSS..247.....M. Retrieved 11 December 2018.
  8. ^ a b c 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" (PDF). The Astrophysical Journal. 791 (2): 11. arXiv:1406.6645. Bibcode:2014ApJ...791..121M. doi:10.1088/0004-637X/791/2/121. Retrieved 11 December 2018.
  9. ^ 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. Retrieved 11 December 2018. (online, AcuA catalog p. 153)
  10. ^ a b c d 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:1109.6407. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. Retrieved 11 December 2018. (catalog)
  11. ^ a b 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. Bibcode:2018MPBu...45..240F. ISSN 1052-8091. Retrieved 11 December 2018.
  12. ^ a b c d "LCDB Data for (1551) Argelander". Asteroid Lightcurve Database (LCDB). Retrieved 11 December 2018.
  13. ^ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 11 December 2018.
  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" (PDF). The Astronomical Journal. 150 (3): 35. arXiv:1504.04041. Bibcode:2015AJ....150...75W. doi:10.1088/0004-6256/150/3/75. Retrieved 11 December 2018.
  15. ^ Durech, J.; Hanus, J.; Oszkiewicz, D.; Vanco, R. (March 2016). "Asteroid models from the Lowell photometric database". Astronomy and Astrophysics. 587: 6. arXiv:1601.02909. Bibcode:2016A&A...587A..48D. doi:10.1051/0004-6361/201527573. Retrieved 11 December 2018.

External links[edit]