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1521 Seinäjoki

From Wikipedia, the free encyclopedia
Main-belt asteroid

1521 Seinäjoki
Shape model of Seinäjoki from itslightcurve
Discovery[1]
Discovered byY. Väisälä
Discovery siteTurku Obs.
Discovery date22 October 1938
Designations
(1521) Seinäjoki
Named after
Seinäjoki(Finnish city)[2]
1938 UB1 · 1933 UR1
1967 UW
main-belt · (outer)[3]
Brasilia[4]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc78.62 yr (28,716 days)
Aphelion3.2435AU
Perihelion2.4633 AU
2.8534 AU
Eccentricity0.1367
4.82yr (1,760 days)
123.44°
0° 12m 16.2s / day
Inclination15.059°
12.593°
48.805°
Physical characteristics
13.66±3.61 km[5]
14.813±0.070 km[6]
16.095±0.070 km[7]
16.29±0.20 km[8]
24.30 km(calculated)[3]
4.32±0.01 h[9]
4.328159±0.000001 h[10]
0.057(assumed)[3]
0.116±0.018[8]
0.1733±0.0300[7]
0.205±0.015[6]
0.22±0.12[5]
C[3]
11.5[7] · 11.8[1][3] · 11.90[8] · 11.92[5] · 12.17±0.45[11]

1521 Seinäjoki (provisional designation1938 UB1) is a Brasiliaasteroid from the outer region of theasteroid belt, approximately 14 kilometers in diameter. It was discovered on 22 October 1938, by Finnish astronomerYrjö Väisälä at the southwesternTurku Observatory, Finland.[12] The asteroid was later named after the Finnish city ofSeinäjoki.[2]

Orbit and classification

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Seinäjoki is a member of theBrasilia family, a smallerasteroid family ofX-type asteroids in theouter main-belt. Since the family's namesake,293 Brasilia, is a suspectedinterloper in its own family, it has also been namedSeinäjoki family after Seinäjoki.[4][13]: 37 

It orbits the Sun in theouter main-belt at a distance of 2.5–3.2 AU once every 4 years and 10 months (1,760 days). Its orbit has aneccentricity of 0.14 and aninclination of 15° with respect to theecliptic.[1] In 1933, Seinäjoki was first identified as1933 UR1 atSimeiz Observatory. The body'sobservation arc, however, begins with its official discovery observation at Turku.[12]

Physical characteristics

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Rotation and pole

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In October 2010, a rotationallightcurve of Seinäjoki was obtained by Russell Durkee at the U.S. Shed of Science Observatory (H39) in Minneapolis. It gave it a well-definedrotation period of 4.32 hours with a brightness variation of 0.15magnitude (U=3).[9] A modeled lightcurve form Lowell photometric database gave a concurring period of 4.328 hours and a spin axis of (-18.0°, 230.0°) inecliptic coordinates.[10]

Diameter and albedo

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According to the survey carried out by NASA'sWide-field Infrared Survey Explorer (WISE) with its subsequentNEOWISE mission, Seinäjoki measures between 13.66 and 14.81 kilometers in diameter, and its surface has analbedo between 0.205 and 0.22 (more recent results only).[5][6][7][8]

TheCollaborative Asteroid Lightcurve Link assumes a standard albedo for carbonaceousC-type asteroids of 0.057 and calculates a much larger diameter of 24.30 kilometers as a body's and diameter and reflectivity (albeo) correlate indirectly.[3] However, based on the much higher albedo given by WISE/NEOWISE, the body is rather of astony composition, which is untypical for asteroids in the outer main-belt.

Naming

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Thisminor planet was named for the city ofSeinäjoki, located inSouthern Ostrobothnia, western Finland.[2] The officialnaming citation was published by theMinor Planet Center on 20 February 1976 (M.P.C. 3929).[14]

References

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  1. ^abcd"JPL Small-Body Database Browser: 1521 Seinajoki (1938 UB1)" (2017-06-05 last obs.).Jet Propulsion Laboratory. Retrieved30 June 2017.
  2. ^abcSchmadel, Lutz D. (2007). "(1521) Seinäjoki".Dictionary of Minor Planet Names.Springer Berlin Heidelberg. p. 121.doi:10.1007/978-3-540-29925-7_1522.ISBN 978-3-540-00238-3.
  3. ^abcdef"LCDB Data for (1521) Seinäjoki". Asteroid Lightcurve Database (LCDB). Retrieved3 January 2017.
  4. ^ab"Asteroid 1521 Seinajoki – Nesvorny HCM Asteroid Families V3.0".Small Bodies Data Ferret. Retrieved26 October 2019.
  5. ^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.
  6. ^abcMasiero, 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. Retrieved3 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.
  8. ^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. Retrieved3 January 2017.
  9. ^abDurkee, Russell I. (January 2011)."Asteroids Observed from the Shed of Science Observatory: 2010 May-October".The Minor Planet Bulletin.38 (1):39–40.Bibcode:2011MPBu...38...39D.ISSN 1052-8091. Retrieved3 January 2017.
  10. ^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. Retrieved3 January 2017.
  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.arXiv:1506.00762.Bibcode:2015Icar..261...34V.doi:10.1016/j.icarus.2015.08.007. Retrieved3 January 2017.
  12. ^ab"1521 Seinajoki (1938 UB1)".Minor Planet Center. Retrieved3 January 2017.
  13. ^Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families".Asteroids IV. pp. 297–321.arXiv:1502.01628.Bibcode:2015aste.book..297N.doi:10.2458/azu_uapress_9780816532131-ch016.ISBN 9780816532131.
  14. ^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.

External links

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