1379 Lomonosowa

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1379 Lomonosowa
001379-asteroid shape model (1379) Lomonosowa.png
Modelled shape of Lomonosowa
Discovery [1]
Discovered by G. Neujmin
Discovery site Simeiz Obs.
Discovery date19 March 1936
Designations
(1379) Lomonosowa
Named after
 Mikhail Lomonosov [2]
(18th century Russian polymath)
1936 FC ·1933 SG1
main-belt  ·(inner)
background [3]
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 111.93 yr (40,882 days)
Aphelion 2.7548 AU
Perihelion 2.2928 AU
2.5238 AU
Eccentricity 0.0915
4.01 yr (1,464 days)
88.814°
0° 14m 44.88s / day
Inclination 15.607°
169.88°
31.359°
Physical characteristics
Dimensions17.82 km (derived) [4]
18.690±0.177 km [5]
19.71±0.80 km [6]
20.135±0.160 km [7]
20.45±0.56 km [8]
24.482±0.0272 h [9]
24.4845±0.0005 h [10]
24.4846±0.0001 h [11]
24.488±0.001 h [12]
24.71 h [13]
0.1584±0.0343 [7]
0.167±0.010 [8]
0.182±0.018 [5]
0.20 (assumed) [4]
0.218±0.021 [6]
S [4] [13]
B–V = 0.830 [1]
U–B = 0.440 [1]
10.626±0.005(R) [9]  ·10.80 [6]  ·10.9 [1]  ·11.05 [8]  ·11.11 [4] [7] [13]  ·11.45±0.27 [14]

    1379 Lomonosowa (prov. designation: 1936 FC) is a stony background asteroid from the central regions of the asteroid belt, approximately 19 kilometers (12 miles) in diameter. Discovered by Grigory Neujmin at the Simeiz Observatory in 1936, the asteroid was later named after Russian physicist and astronomer Mikhail Lomonosov. [2] [15]

    Contents

    Discovery

    Lomonosowa was discovered on 19 March 1936, by Soviet astronomer Grigory Neujmin at the Simeiz Observatory on the Crimean peninsula. [15] On the same night, it was independently discovered by Serbian astronomer Petar Đurković at Uccle Observatory in Belgium. [2] The Minor Planet Center only recognizes the first discoverer. [15] A first precovery of Lomonosowa was taken at the Lowell Observatory in October 1905. The asteroid was first identified as 1933 SG1 at Heidelberg Observatory in September 1933. [15]

    Orbit and classification

    Lomonosowa is a non-family asteroid of the main belt's background population. [3] It orbits the Sun in the central asteroid belt at a distance of 2.3–2.8  AU once every 4.01 years (1,464 days). Its orbit has an eccentricity of 0.09 and an inclination of 16° with respect to the ecliptic. [1] The body's observation arc begins with its first precovery at Lowell Observatory in October 1905. [15]

    Naming

    This minor planet was named after Russian physicist and astronomer Mikhail Lomonosov (1711–1765). He discovered the atmosphere of Venus and the principle of mass conservation. [2] The official naming citation was published by the Minor Planet Center in June 1955 ( M.P.C. 1252). [16] He is also honored by the craters Lomonosov on the Moon and Lomonosov on Mars. [2]

    Physical characteristics

    Lomonosowa has been characterized as a common, stony S-type asteroid. [13]

    Lightcurves

    Several rotational lightcurve of Lomonosowa have been obtained from photometric observations since the 1980s. Lightcurve analysis gave a rotation period between 24.482 and 24.71 hours with a brightness amplitude of 0.45 to 0.63 magnitude ( U=2/3/2 ). [9] [12] [13] The asteroid's lightcurve has also been modeled using photometric observations from various sources. Modelling gave a concurring sidereal period of 24.4845 and 24.4846 hours. [10] [11] One study also found two spin axis of (72.0°, −84.0°) and (265.0°, −46.0°) in ecliptic coordinates (λ, β). [11]

    Diameter and albedo

    According to the surveys carried out by the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Lomonosowa measures between 18.690 and 20.45 kilometers in diameter and its surface has an albedo between 0.1584 and 0.218. [5] [6] [7] [8] The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and derives a diameter of 17.82 kilometers based on an absolute magnitude of 11.11. [4]

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    References

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    6. 1 2 3 4 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 . Retrieved 27 October 2017.
    7. 1 2 3 4 Mainzer, 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. 1 2 3 4 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)
    9. 1 2 3 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 . Retrieved 27 October 2017.
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    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 . Retrieved 27 October 2017.
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    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. doi:10.1007/978-3-642-01965-4. ISBN   978-3-642-01964-7.
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