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1449 Virtanen

From Wikipedia, the free encyclopedia
Main-belt asteroid

1449 Virtanen
Shape ofVirtanen modelled from itslightcurve
Discovery[1]
Discovered byY. Väisälä
Discovery siteTurku Obs.
Discovery date20 February 1938
Designations
(1449) Virtanen
Named after
Artturi Virtanen(biochemist)[2]
1938 DO · 1928 DC
main-belt · Flora[3]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc89.10 yr (32,543 days)
Aphelion2.5378AU
Perihelion1.9069 AU
2.2223 AU
Eccentricity0.1419
3.31yr (1,210 days)
289.08°
0° 17m 51s / day
Inclination6.6413°
110.78°
132.16°
Physical characteristics
Dimensions9.15±1.91 km[4]
9.263±0.098 km[5]
9.46±0.33 km[6]
9.947±0.092 km[7]
10.31 km(calculated)[3]
14.770±0.440h(R)[8]
30.495±0.005 h[9]
30.5±0.5 h[10]
30.5005±0.0005 h[11]
30.5006±0.0001 h[12]
30.52±0.01 h[10]
30.5421±0.7655 h(R)[13]
30.5465±0.3727 h(S)[13]
0.24(assumed)[3]
0.285±0.038[6]
0.2856±0.0274[7]
0.36±0.15[4]
Tholen =S[1] · S[3]
11.690±0.150(R)[8] · 11.779±0.003(R)[13] · 12.0[7] · 12.1[1][3][6] · 12.25[4] · 12.615±0.004(S)[13] · 13.21±0.09[14]

1449 Virtanen, provisional designation1938 DO, is a stony Florianasteroid from the inner regions of theasteroid belt, approximately 9.2 kilometers in diameter. It was discovered on 20 February 1938, by Finnish astronomerYrjö Väisälä atTurku Observatory in Southwest Finland,[15] and named for Finnish biochemistArtturi Virtanen.[2]

Description

[edit]

Virtanen is a member of theFlora family, one of the largest collisional populations of stony asteroids in the main-belt. It orbits the Sun in theinner main-belt at a distance of 1.9–2.5 AU once every 3 years and 4 months (1,210 days). Its orbit has aneccentricity of 0.14 and aninclination of 7° with respect to theecliptic.[1] In 1928,Virtanen was first identified as1928 DC atHeidelberg, extending the body'sobservation arc by 10 years prior to its official discovery at Turku.[15]

Physical characteristics

[edit]

In theTholen taxonomy,Virtanen is classified as a commonS-type asteroid.[1]

Lightcurves

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Virtanen's first rotationallightcurve was obtained by astronomersPierre Antonini andSilvano Casulli in May 2007, followed by Australian astronomer Julian Oey at Leura (E17) and Kingsgrove Observatory (E19) in June 2008. The lightcurves gave arotation period of approximately 30.5 hours with a brightness variation of 0.6magnitude (U=2-/3-/3-).[9][10]

Additional periods were obtained from photometric observation in the R and S-band at thePalomar Transient Factory (U=2/2/2),[8][13] and from modeled data using the Lowell photometric database and other data sources, which also gave two spin axis of (307.0°, 58.0°) and (89.0°, 61.0°) inecliptic coordinates, respectively (U=n.a.).[11][12]

Diameter and albedo

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According to the survey carried out by NASA'sWide-field Infrared Survey Explorer with its subsequentNEOWISE mission,Virtanen measures between 9.15 and 9.947 kilometers in diameter, and its surface has analbedo between 0.285 and 0.36.[4][5][6][7]

TheCollaborative Asteroid Lightcurve Link assumes an albedo of 0.24 – derived from8 Flora, the largest member and namesake of its family – and calculates a diameter of 10.31 kilometers with anabsolute magnitude of 12.1.[3]

Naming

[edit]

Thisminor planet was named for famous Finnish biochemistArtturi Virtanen (1895–1973), recipient of the 1945Nobel Prize in Chemistry and president of theAcademy of Finland for many years.[2] The officialnaming citation was published by theMinor Planet Center on 15 February 1970 (M.P.C. 3023).[16]

References

[edit]
  1. ^abcdef"JPL Small-Body Database Browser: 1449 Virtanen (1938 DO)" (2017-03-31 last obs.).Jet Propulsion Laboratory. Retrieved25 July 2017.
  2. ^abcSchmadel, Lutz D. (2007). "(1449) Virtanen".Dictionary of Minor Planet Names – (1449) Virtanen.Springer Berlin Heidelberg. p. 116.doi:10.1007/978-3-540-29925-7_1450.ISBN 978-3-540-00238-3.
  3. ^abcdef"LCDB Data for (1449) Virtanen". Asteroid Lightcurve Database (LCDB). Retrieved4 January 2017.
  4. ^abcdNugent, C. R.; Mainzer, A.; Bauer, J.; Cutri, R. M.; Kramer, E. A.; Grav, T.; et al. (September 2016)."NEOWISE Reactivation Mission Year Two: Asteroid Diameters and Albedos".The Astronomical Journal.152 (3): 12.arXiv:1606.08923.Bibcode:2016AJ....152...63N.doi:10.3847/0004-6256/152/3/63.
  5. ^abMasiero, 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:1406.6645.Bibcode:2014ApJ...791..121M.doi:10.1088/0004-637X/791/2/121.S2CID 119293330. Retrieved4 January 2017.
  6. ^abcdMasiero, 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.arXiv:1209.5794.Bibcode:2012ApJ...759L...8M.doi:10.1088/2041-8205/759/1/L8.S2CID 46350317. Retrieved4 January 2017.
  7. ^abcdMainzer, 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.arXiv:1109.6407.Bibcode:2011ApJ...741...90M.doi:10.1088/0004-637X/741/2/90.S2CID 35447010.
  8. ^abcChang, Chan-Kao;Ip, Wing-Huen; Lin, Hsing-Wen; Cheng, Yu-Chi; Ngeow, Chow-Choong; Yang, Ting-Chang; et al. (August 2015)."Asteroid Spin-rate Study Using the Intermediate Palomar Transient Factory".The Astrophysical Journal Supplement Series.219 (2): 19.arXiv:1506.08493.Bibcode:2015ApJS..219...27C.doi:10.1088/0067-0049/219/2/27.S2CID 17093124. Retrieved4 January 2017.
  9. ^abOey, Julian (October 2009)."Lightcurve Analysis of Asteroids from Leura and Kingsgrove Observatory in the Second Half of 2008".The Minor Planet Bulletin.36 (4):162–164.Bibcode:2009MPBu...36..162O.ISSN 1052-8091. Retrieved4 January 2017.
  10. ^abcBehrend, Raoul."Asteroids and comets rotation curves – (1449) Virtanen".Geneva Observatory. Retrieved4 January 2017.
  11. ^abHanus, J.; Durech, J.; Oszkiewicz, D. A.; Behrend, R.; Carry, B.; Delbo, M.; et al. (February 2016). "New and updated convex shape models of asteroids based on optical data from a large collaboration network".Astronomy and Astrophysics.586: 24.arXiv:1510.07422.Bibcode:2016A&A...586A.108H.doi:10.1051/0004-6361/201527441.S2CID 119112278.
  12. ^abDurech, 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.S2CID 118427201. Retrieved4 January 2017.
  13. ^abcdeWaszczak, 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:1504.04041.Bibcode:2015AJ....150...75W.doi:10.1088/0004-6256/150/3/75.S2CID 8342929. Retrieved4 January 2017.
  14. ^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:1506.00762.Bibcode:2015Icar..261...34V.doi:10.1016/j.icarus.2015.08.007.S2CID 53493339. Retrieved4 January 2017.
  15. ^ab"1449 Virtanen (1938 DO)".Minor Planet Center. Retrieved4 January 2017.
  16. ^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.Bibcode:2009dmpn.book.....S.doi:10.1007/978-3-642-01965-4.ISBN 978-3-642-01964-7.

External links

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