1450 Raimonda

From Wikipedia, the free encyclopedia
Jump to navigation Jump to search
1450 Raimonda
1450Raimonda (Lightcurve Inversion).png
Lightcurve-based 3D-model of Raimonda
Discovery [1]
Discovered by Y. Väisälä
Discovery site Turku Obs.
Discovery date 20 February 1938
MPC designation (1450) Raimonda
Named after
Jean Jacques Raimond, Jr.[2]
(Dutch astronomer)
1938 DP · 1934 GJ
A915 TF
main-belt · (middle)[3]
background [4]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 101.96 yr (37,242 days)
Aphelion 3.0591 AU
Perihelion 2.1642 AU
2.6117 AU
Eccentricity 0.1713
4.22 yr (1,542 days)
0° 14m 0.6s / day
Inclination 4.8635°
Physical characteristics
Dimensions 14.75 km (derived)[3]
14.76±4.56 km[5]
14.88±0.9 km[6]
18.481±0.084 km[7]
18.700±0.068 km[8]
20.80±1.15 km[9]
12.6344 h[10]
12.66 h[11]
0.0976 (derived)[3]
S (assumed)[3]
11.90[6][8][9] · 12.30[1][3][5]

1450 Raimonda, provisional designation 1938 DP, is a background asteroid from the central regions of the asteroid belt, approximately 15 kilometers in diameter. It was discovered on 20 February 1938, by astronomer Yrjö Väisälä at the Iso-Heikkilä Observatory in Turku, Finland.[12] The asteroid was named after Dutch astronomer Jean Jacques Raimond, Jr..[2]

Orbit and classification[edit]

Raimonda is a non-family asteroid of the main belt's background population.[4] It orbits the Sun in the central asteroid belt at a distance of 2.2–3.1 AU once every 4 years and 3 months (1,542 days). Its orbit has an eccentricity of 0.17 and an inclination of 5° with respect to the ecliptic.[1]

The body's observation arc begins with its first identification as A915 TF at Heidelberg Observatory in October 1915, more than 22 years prior to its official discovery observation at Turku.[12]

Physical characteristics[edit]

Raimonda is an assumed stony S-type asteroid,[3] despite its rather low albedo.

Rotation period and poles[edit]

In December 2004, a rotational lightcurve of Raimonda was obtained from photometric observations at the Oakley (916) and Tenagra Observatory (848). Lightcurve analysis gave a rotation period of 12.66 hours with a brightness amplitude of 0.64 (or 0.57 at LCDB) magnitude (U=2), indicative of an elongated shape.[11]

In 2013, a lightcurve was modeled from photometric data collected by the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory survey, and individual observers, as well as sparse-in-time photometry from the United States Naval Observatory Flagstaff Station, the Catalina Sky Survey in Tucson, and the Roque de los Muchachos Observatory at La Palma. Modelling gave a similar period 12.6344 hours. The study also determined two spin axis of (231.0°, −56.0°) and (71.0°, −60.0°) in ecliptic coordinates (λ, β).[10]

Diameter and albedo[edit]

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, Raimonda measures between 14.76 and 20.80 kilometers in diameter and its surface has an albedo between 0.074 and 0.1387.[5][6][7][8][9]

The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0976 and a diameter of 14.75 kilometers based on an absolute magnitude of 12.3.[3]


This minor planet was named after Jean Jacques Raimond, Jr. (1903–1961), a Dutch astronomer who was the president of the Dutch Astronomical Society (Dutch: Nederlandse Vereniging voor Weer- en Sterrenkunde; Netherlands Association for Meteorology and Astronomy) and director of the Zeiss planetarium at The Hague.[2]

The naming was suggested by Belgian astronomer Jean Meeus, and the citation was published by the Minor Planet Center before November 1977 (M.P.C. 2347).[13] The lunar crater Raimond was also named in his honor.[2]


  1. ^ a b c d "JPL Small-Body Database Browser: 1450 Raimonda (1938 DP)" (2017-10-01 last obs.). Jet Propulsion Laboratory. Retrieved 21 October 2017. 
  2. ^ a b c d Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (1450) Raimonda. Springer Berlin Heidelberg. p. 116. ISBN 978-3-540-00238-3. Retrieved 21 October 2017. 
  3. ^ a b c d e f g "LCDB Data for (1450) Raimonda". Asteroid Lightcurve Database (LCDB). Retrieved 21 October 2017. 
  4. ^ a b "Small Bodies Data Ferret". Nesvorny HCM Asteroid Families V3.0. Retrieved 21 October 2017. 
  5. ^ a b c d Nugent, C. R.; Mainzer, A.; Masiero, J.; Bauer, J.; Cutri, R. M.; Grav, T.; et al. (December 2015). "NEOWISE Reactivation Mission Year One: Preliminary Asteroid Diameters and Albedos". The Astrophysical Journal. 814 (2): 13. arXiv:1509.02522Freely accessible. Bibcode:2015ApJ...814..117N. doi:10.1088/0004-637X/814/2/117. Retrieved 21 October 2017. 
  6. ^ a b c d 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. Archived from the original on 2016-06-03. Retrieved 21 October 2017. 
  7. ^ 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". The Astrophysical Journal. 791 (2): 11. arXiv:1406.6645Freely accessible. Bibcode:2014ApJ...791..121M. doi:10.1088/0004-637X/791/2/121. Retrieved 21 October 2017. 
  8. ^ 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:1109.6407Freely accessible. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. Retrieved 21 October 2017. 
  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 21 October 2017. 
  10. ^ a b Hanus, J.; Durech, J.; Broz, M.; Marciniak, A.; Warner, B. D.; Pilcher, F.; et al. (March 2013). "Asteroids' physical models from combined dense and sparse photometry and scaling of the YORP effect by the observed obliquity distribution" (PDF). Astronomy and Astrophysics. 551: 16. arXiv:1301.6943Freely accessible. Bibcode:2013A&A...551A..67H. doi:10.1051/0004-6361/201220701. Retrieved 21 October 2017. 
  11. ^ a b Lecrone, Crystal; Addleman, Don; Butler, Thomas; Hudson, Erin; Mulvihill, Alex; Reichert, Chris; et al. (September 2005). "2004-2005 winter observing campaign at Rose-Hulman Institute: results for 1098 Hakone, 1182 Ilona, 1294 Antwerpia, 1450 Raimonda, 2251 Tikhov, and 2365 Interkosmos". The Minor Planet Bulletin. 32 (3): 46–48. Bibcode:2005MPBu...32...46L. ISSN 1052-8091. Retrieved 21 October 2017. 
  12. ^ a b "1450 Raimonda (1938 DP)". Minor Planet Center. Retrieved 21 October 2017. 
  13. ^ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 21 October 2017. 

External links[edit]