4150 Starr
Discovery [1]
Discovered byB. A. Skiff
Discovery siteAnderson Mesa Stn.
Discovery date31 August 1984
Designations
(4150) Starr
Named after
Richard Starkey
(Ringo Starr, The Beatles)[2]
1984 QC1 · 1957 KG
1964 RH · 1973 FD2
1974 QM1 · 1980 EA2
1981 TO2 · 1981 WE6
1981 WJ3 · 1988 YC
2004 SL12
main-belt · Flora [3]
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc60.02 yr (21,922 days)
Aphelion2.6034 AU
Perihelion1.8620 AU
2.2327 AU
Eccentricity0.1660
3.34 yr (1,219 days)
332.80°
0° 17m 43.44s / day
Inclination3.1948°
122.92°
197.41°
Physical characteristics
Dimensions6.641±0.032[4]
6.903±0.050 km[5]
7.47 km (calculated)[3]
4.5179±0.0005 h[6][lower-alpha 1]
6.8 h[7]
0.24 (assumed)[3]
0.2584±0.0469[5]
0.277±0.023[4]
S [3][8]
12.50±0.48[8] · 12.8[1][3] · 12.9[5]

    4150 Starr, provisional designation 1984 QC1, is a stony Florian asteroid from the inner regions of the asteroid belt, approximately 7 kilometers in diameter. It was discovered by American astronomer Brian Skiff at Lowell's Anderson Mesa Station on 31 August 1984.[9] It was named after musician Ringo Starr.[2]

    Orbit and classification

    Starr is a member of the Flora family, one of the largest groups of stony asteroids in the main-belt. It orbits the Sun in the inner main-belt at a distance of 1.9–2.6 AU once every 3 years and 4 months (1,219 days). Its orbit has an eccentricity of 0.17 and an inclination of 3° with respect to the ecliptic.[1] The first observation was made at the U.S. Goethe Link Observatory in 1957, extending the asteroid's observation arc by 27 years prior to its discovery.[9]

    Physical characteristics

    Starr has been characterized as a common S-type asteroid by PanSTARRS' photometric survey.[3][8]

    Rotation period

    According to the space-based survey by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Starr measures 6.6 and 6.9 kilometers in diameter and its surface has an albedo of 0.258 and 0.277, respectively,[4][5] while the Collaborative Asteroid Lightcurve Link (CALL) assumes an albedo of 0.24 – derived from 8 Flora, the family's largest member and namesake – and calculates a diameter of 7.5 kilometers with an absolute magnitude of 12.8.[3]

    Diameter and albedo

    Several rotational lightcurves of Starr were obtained from photometric observations. An unpublished lightcurve by Kryszczynska from November 2011, has been rated best by CALL.[3] It gave a rotation period of 4.5179±0.0005 hours and a brightness variation of 0.20 in magnitude (U=3).[lower-alpha 1]

    Naming

    This minor planet was named after Richard Starkey (born 1940), better known as Ringo Starr, the drummer of The Beatles. He joined the English rock band in 1962, replacing its former drummer Pete Best. Ringo has released various albums in his solo career and also acted in several movies.[2] The official naming citation was published by the Minor Planet Center on 10 April 1990 (M.P.C. 16248).[10] The minor planets 8749 Beatles, 4147 Lennon, 4148 McCartney and 4149 Harrison were named after the band and its three other members.

    Notes

    1. 1 2 Kryszczynska (2012a), unpublished data: rotation period 4.5179±0.0005 hours with a brightness amplitude of 0.20 mag. CALL rates the light-curve as well-defined on its quality scheme. Summary figures for (4150) Starr at Collaborative Asteroid Lightcurve Link (CALL)

    References

    1. 1 2 3 4 "JPL Small-Body Database Browser: 4150 Starr (1984 QC1)" (2017-06-05 last obs.). Jet Propulsion Laboratory. Retrieved 20 June 2017.
    2. 1 2 3 Schmadel, Lutz D. (2007). "(4150) Starr". Dictionary of Minor Planet Names – (4150) Starr. Springer Berlin Heidelberg. p. 355. doi:10.1007/978-3-540-29925-7_4122. ISBN 978-3-540-00238-3.
    3. 1 2 3 4 5 6 7 8 "LCDB Data for (4150) Starr". Asteroid Lightcurve Database (LCDB). Retrieved 16 August 2016.
    4. 1 2 3 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:1406.6645. Bibcode:2014ApJ...791..121M. doi:10.1088/0004-637X/791/2/121. S2CID 119293330. Retrieved 5 December 2016.
    5. 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. S2CID 35447010.
    6. ↑ Bianchi, E. (December 1920). "Osservazioni fotometriche di pianeti". Memorie della Società Astronomia Italiana. 2: 45. Bibcode:1921MmSAI...2...45B. Retrieved 16 August 2016.
    7. ↑ Angeli, C. A.; Guimarã; es, T. A.; Lazzaro, D.; Duffard, R.; Fernández, S.; et al. (April 2001). "Rotation Periods for Small Main-Belt Asteroids From CCD Photometry". The Astronomical Journal. 121 (4): 2245–2252. Bibcode:2001AJ....121.2245A. doi:10.1086/319936.
    8. 1 2 3 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 16 August 2016.
    9. 1 2 "4150 Starr (1984 QC1)". Minor Planet Center. Retrieved 16 August 2016.
    10. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 16 August 2016.
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