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1889 Pakhmutova

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1889 Pakhmutova
Lightcurve-based 3D-model of Pakhmutova
Discovery[1]
Discovered byL. Chernykh
Discovery siteCrimean Astrophysical Obs.
Discovery date24 January 1968
Designations
(1889) Pakhmutova
Named after
Aleksandra Pakhmutova
(Russian composer)[2]
1968 BE · 1942 JM
1966 US · 1969 JM
main-belt · (outer)[3]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc50.53 yr (18,455 days)
Aphelion3.4349 AU
Perihelion2.7452 AU
3.0901 AU
Eccentricity0.1116
5.43 yr (1,984 days)
33.156°
0° 10m 53.04s / day
Inclination13.183°
55.153°
84.606°
Physical characteristics
Dimensions33.41 km (derived)[3]
33.53±1.8 km[4]
35.24±0.63 km[5]
35.45±10.87 km[6]
37.47±0.84 km[7]
37.68±14.19 km[8]
17.490±0.004 h[9][a]
17.5157±0.0005 h[10]
17.5226±0.0113 h[11]
0.05±0.04[8]
0.057±0.013[5]
0.0574 (derived)[3]
0.06±0.09[6]
0.061±0.003[7]
0.0752±0.009[4]
C[3]
10.80[4][7] · 10.969±0.002 (R)[11] · 11.0[5][8] · 11.1[1][3] · 11.12[6] · 11.29±0.37[12]

1889 Pakhmutova, provisional designation 1968 BE, is a carbonaceous asteroid from the outer region of the asteroid belt, approximately 35 kilometers in diameter.

It was discovered by Russian astronomer Lyudmila Chernykh at the Crimean Astrophysical Observatory in Nauchnyj on 24 January 1968.[13] The asteroid was named after Russian composer Aleksandra Pakhmutova.[2]

Orbit and classification

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Pakhmutova orbits the Sun in the outer main-belt at a distance of 2.7–3.4 AU once every 5 years and 5 months (1,984 days). Its orbit has an eccentricity of 0.11 and an inclination of 13° with respect to the ecliptic.[1] It was first identified as 1942 JM at Johannesburg Observatory in 1942. Its first used observation was made in 1968, when it was identified as 1966 US at the discovering observatory, extending the body's observation arc by 2 years prior to its official discovery observation.[13]

Physical characteristics

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Pakhmutova has been characterized as a carbonaceous C-type asteroid.[3]

Diameter and albedo

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This asteroid has a mean-diameter between 33.53 and 37.68 kilometers, and an albedo between 0.05 and 0.0752, as measured by the space-based Akari, IRAS and WISE/NEOWISE surveys.[4][5][6][7][8] The Collaborative Asteroid Lightcurve Link derives an albedo of 0.0574 and a diameter of 33.41 kilometers with an absolute magnitude of 11.1.[3]

Rotation period and poles

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In February 2006, a rotational lightcurve[a] was obtained by American astronomer Brian Warner at his Palmer Divide Observatory (716) in Colorado. Lightcurve analysis gave a rotation period of 17.490 hours with a brightness variation of 0.50 in magnitude (U=3-).[9] Photometric observations at the Palomar Transient Factory in February 2012, gave a period of 17.5226 hours and an amplitude of 0.49 magnitude (U=2).[11]

In 2011, a modeled lightcurve using data from the Uppsala Asteroid Photometric Catalogue (UAPC) and other sources gave a period 17.5157 hours, as well as a spin axis of (22.0°, –76.0°; 167.0°, –40.0°) in ecliptic coordinates (λ, β) (U=2).[10]

Naming

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This minor planet was named in honor of the Russian composer Aleksandra Pakhmutova, one of the best known figures in Soviet and later Russian popular music.[2] The official naming citation was published by the Minor Planet Center on 20 February 1976 (M.P.C. 3936).[14]

Notes

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  1. ^ a b Lightcurve plot of 1889 Pakhmutova with a rotation period 17.490±0.004 hours with a brightness amplitude of 0.50±0.02 by B. D. Warner at the Palmer Divide Observatory (2006). Summary figures at LCDB

References

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  1. ^ a b c d "JPL Small-Body Database Browser: 1889 Pakhmutova (1968 BE)" (2017-04-30 last obs.). Jet Propulsion Laboratory. Retrieved 9 June 2017.
  2. ^ a b c Schmadel, Lutz D. (2007). "(1889) Pakhmutova". Dictionary of Minor Planet Names – (1889) Pakhmutova. Springer Berlin Heidelberg. p. 151. doi:10.1007/978-3-540-29925-7_1890. ISBN 978-3-540-00238-3.
  3. ^ a b c d e f g "LCDB Data for (1889) Pakhmutova". Asteroid Lightcurve Database (LCDB). Retrieved 11 December 2016.
  4. ^ 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 – IRAS-A-FPA-3-RDR-IMPS-V6.0. Bibcode:2004PDSS...12.....T. Retrieved 17 October 2019.
  5. ^ 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". The Astrophysical Journal Letters. 759 (1): 5. arXiv:1209.5794. Bibcode:2012ApJ...759L...8M. doi:10.1088/2041-8205/759/1/L8. S2CID 46350317. Retrieved 11 December 2016.
  6. ^ a b c d Nugent, 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.
  7. ^ 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. (online, AcuA catalog p. 153)
  8. ^ 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:1509.02522. Bibcode:2015ApJ...814..117N. doi:10.1088/0004-637X/814/2/117. S2CID 9341381. Retrieved 9 June 2017.
  9. ^ a b Warner, Brian D. (December 2006). "Asteroid lightcurve analysis at the Palmer Divide Observatory - February - March 2006". The Minor Planet Bulletin. 33 (4): 82–84. Bibcode:2006MPBu...33...82W. ISSN 1052-8091. Retrieved 11 December 2016.
  10. ^ a b Hanus, J.; Durech, J.; Broz, M.; Warner, B. D.; Pilcher, F.; Stephens, R.; et al. (June 2011). "A study of asteroid pole-latitude distribution based on an extended set of shape models derived by the lightcurve inversion method". Astronomy & Astrophysics. 530: 16. arXiv:1104.4114. Bibcode:2011A&A...530A.134H. doi:10.1051/0004-6361/201116738. Retrieved 11 December 2016.
  11. ^ a b c 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. arXiv:1504.04041. Bibcode:2015AJ....150...75W. doi:10.1088/0004-6256/150/3/75. S2CID 8342929. Retrieved 11 December 2016.
  12. ^ 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. Retrieved 11 December 2016.
  13. ^ a b "1889 Pakhmutova (1968 BE)". Minor Planet Center. Retrieved 11 December 2016.
  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. Bibcode:2009dmpn.book.....S. doi:10.1007/978-3-642-01965-4. ISBN 978-3-642-01964-7.
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