3043 San Diego

3043 San Diego, provisional designation 1982 SA, is a stony Hungaria asteroid and slow rotator from the inner regions of the asteroid belt, approximately 4.7 kilometers in diameter.

3043 San Diego
Discovery [1]
Discovered byE. F. Helin
Discovery sitePalomar Obs.
Discovery date20 September 1982
Designations
(3043) San Diego
Named after
San Diego (city)[2]
1982 SA · 1974 SQ2
main-belt[1] · Hungaria [3][4][5]
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc41.90 yr (15,305 days)
Aphelion2.1323 AU
Perihelion1.7210 AU
1.9266 AU
Eccentricity0.1067
2.67 yr (977 days)
7.5114°
0° 22m 6.96s / day
Inclination21.788°
351.11°
31.747°
Physical characteristics
Dimensions4.62 km (calculated)[4]
4.771±0.022 km[6]
5.040±0.082 km[7]
30.72±0.02 h (wrong)[8]
105.7±0.1 h (re-examined)[9]
0.252±0.048[7]
0.2817±0.0408[6]
0.30 (assumed)[4]
E [4]
13.6[1][6] · 13.7[4]

    It was discovered by American astronomer Eleanor Helin on 30 September 1982, at the U.S. Palomar Observatory in California, and named for the city of San Diego.[2][3]

    Classification and orbit

    The bright E-type asteroid is a member of the Hungaria family, which form the innermost dense concentration of asteroids in the Solar System. The asteroid orbits the Sun at a distance of 1.7–2.1 AU once every 2 years and 8 months (977 days). Its orbit has an eccentricity of 0.11 and an inclination of 22° with respect to the ecliptic.[1] The first observation was taken at Crimea–Nauchnij in 1974, extending the asteroid's observation arc by 8 years prior to its discovery.[3]

    Slow rotator

    San Diego is a slow rotator. In March 2005, a rotational lightcurve was obtained from photometric observations by American astronomer Brian Warner at his Palmer Divide Observatory (716) in Colorado. It gave a long rotation period of 105.7 hours with a brightness variation of 0.60 in magnitude (U=3-). The period was derived from a re-examined lightcurve that originally gave a much shorter period of 30.72±0.02 hours with an amplitude of 0.37 in magnitude (U=0).[8] This previously published period was only preliminary and is now considered wrong upon re-examination.[4]

    Diameter and albedo

    According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, San Diego measures 4.8 and 5.0 kilometers in diameter and its surface has an albedo of 0.25 and 0.28, respectively,[6][7] while the Collaborative Asteroid Lightcurve Link assumes an albedo of 0.30 – a compromise value between 0.4 and 0.2, corresponding to the Hungaria asteroids both as family and orbital group – and calculates a diameter of 4.6 kilometers with an absolute magnitude of 13.7.[4]

    Naming

    This minor planet was named for the city of San Diego, California, in appreciation of the city council's efforts to reduce the local light pollution (see dark-sky movement). Palomar mountain is located within San Diego County, California, and the astronomers at the site were concerned that the light pollution from the city would ruin their ability to use the observatory. The council had voted to use Low-Pressure Sodium (LPS) vapor lamps for their street lights. This fixture only emitted light at one wavelength, which astronomers could readily filter out.[2] The approved naming citation was published by the Minor Planet Center on 13 July 1984 (M.P.C. 8914).[10]

    References
    1. "JPL Small-Body Database Browser: 3043 San Diego (1982 SA)" (2016-08-15 last obs.). Jet Propulsion Laboratory. Retrieved 3 July 2017.
    2. Schmadel, Lutz D. (2007). "(3043) San Diego". Dictionary of Minor Planet Names – (3043) San Diego. Springer Berlin Heidelberg. p. 251. doi:10.1007/978-3-540-29925-7_3044. ISBN 978-3-540-00238-3.
    3. "3043 San Diego (1982 SA)". Minor Planet Center. Retrieved 21 August 2016.
    4. "LCDB Data for (3043) San Diego". Asteroid Lightcurve Database (LCDB). Retrieved 21 August 2016.
    5. Spratt, Christopher E. (April 1990). "The Hungaria group of minor planets". Journal of the Royal Astronomical Society of Canada. 84 (2): 123–131. Bibcode:1990JRASC..84..123S. ISSN 0035-872X.
    6. 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. Retrieved 21 August 2016.
    7. 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. Retrieved 6 December 2016.
    8. Warner, Brian D. (September 2005). "Asteroid lightcurve analysis at the Palmer Divide Observatory - winter 2004-2005". The Minor Planet Bulletin. 32 (3): 54–58. Bibcode:2005MPBu...32...54W. ISSN 1052-8091. Retrieved 7 January 2016.
    9. Warner, Brian D.; Stephens, Robert, D.; Harris, Alan W.; Pravec, Petr (October 2009). "A Re-examination of the Lightcurves for Seven Hungaria Asteroids". The Minor Planet Bulletin. 36 (4): 176–179. Bibcode:2009MPBu...36..176W. ISSN 1052-8091. Retrieved 7 January 2016.
    10. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 21 August 2016.

    Further reading

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