1355 Magoeba

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1355 Magoeba
Discovery [1]
Discovered by C. Jackson
Discovery site Johannesburg Obs.
Discovery date30 April 1935
Designations
(1355) Magoeba
Named after
Magoeba
(South African chief) [2]
1935 HE
main-belt  · Hungaria [3] [4]
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 81.71 yr (29,843 days)
Aphelion 1.9363 AU
Perihelion 1.7707 AU
1.8535 AU
Eccentricity 0.0447
2.52 yr (922 days)
245.86°
0° 23m 26.16s / day
Inclination 22.827°
225.25°
340.40°
Physical characteristics
Dimensions4.276±0.170 km [5]
4.828±0.094 km [6]
5.96 km (calculated) [4]
2.9712±0.0003 h [7]
2.972±0.002 h [8]
2.975±0.002 h [8]
5.946±0.005 h [9]
5.99±0.05 h [10] [lower-alpha 1]
31.65±0.05 h [9]
32.9±0.1 h [11]
0.267±0.095 [12]
0.3 (assumed) [4]
0.4663±0.0824 [6]
0.582±0.049 [5]
Tholen = X [1]  · M [13]  · E [6]  · X [4]
B–V = 0.713 [1]
U–B = 0.255 [1]
13.02±0.22 [14]  ·13.05 [1] [4] [6]

    1355 Magoeba, provisional designation 1935 HE, is a Hungaria asteroid and a suspected contact-binary from the innermost regions of the asteroid belt, approximately 5 kilometers in diameter. It was discovered on 30 April 1935, by English-born, South African astronomer Cyril Jackson at the Johannesburg Observatory in South Africa. [3] The asteroid is named for Magoeba, a tribal chief in the South African Transvaal Province. [2]

    Contents

    Orbit and classification

    Magoeba is a member of the Hungaria family, which forms the innermost dense concentration of asteroids in the Solar System. It orbits the Sun in the inner main-belt at a distance of 1.8–1.9  AU once every 2 years and 6 months (922 days). Its orbit has an eccentricity of 0.04 and an inclination of 23° with respect to the ecliptic. [1] The first precovery was taken at Nice Observatory just 3 day prior to its official discovery. The body's observation arc begins at Johannesburg the night after its discovery observation. [3]

    Physical characteristics

    Lightcurves

    Between 2006 and 2014, several rotational lightcurves of Magoeba were obtained by American astronomer Brian Warner at the CS3–Palmer Divide Station ( U82 ) in California. Lightcurve analysis of the photometric observations taken during the asteroid's 2014-apparition gave a rotation period of 2.971 hours with a brightness variation of 0.09 magnitude ( U=3 ). [7] [lower-alpha 2]

    Previously derived periods varied strongly (5.99 and 31.65 hours) with alternative period solutions ( U=2-/2/2 ). [9] [10] [11] [lower-alpha 1] The Observation were taken at the Palmer Divide Observatory ( 716 ) in Colorado (see video in § External links). It is now suspected that this discrepancy might be caused by the presence of an asteroid moon that orbits Magoeba with a period of 15.05 hours. [7]

    Diameter and albedo

    According to the survey carried out by NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Magoeba measures 4.276 and 4.828 kilometers in diameter, and its surface has an albedo of 0.582 and 0.466, respectively, [5] [6] while a polarimetric study of Hungaria asteroids found a lower albedo of 0.267. [12] 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 5.96 kilometers with an absolute magnitude of 13.05. [4]

    Spectral type

    In the Tholen taxonomy, Magoeba is an X-type asteroid, which can be further divided into the bright E, the metallic M and the carbonaceous P classes, with similar spectra but very different inferred mineralogies. [13] It has both been classified as an E-type asteroid by the WISE/NEOWISE mission, and as a M-type asteroid by a dedicated spectroscopic survey at the Argentinian Lencito Complex, respectively. [6] [13]

    Naming

    This minor planet was named for Magoeba, a native chief of the North Transvaal in South Africa. [2] The official naming citation was published by the Minor Planet Center in April 1953 ( M.P.C. 908). [15]

    Notes

    1. 1 2 Lightcurve plot of (1355) Magoeba, Palmer Divide Observatory, B. D. Warner (2011)
    2. ↑ Light-curve plots of (1355) Magoeba from the 2013-observation and from the 2014-observation, published by the Center for Solar System Studies (CS3) in Landers, California.

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    References

    1. 1 2 3 4 5 6 7 "JPL Small-Body Database Browser: 1355 Magoeba (1935 HE)" (2017-01-09 last obs.). Jet Propulsion Laboratory . Retrieved 25 July 2017.
    2. 1 2 3 Schmadel, Lutz D. (2007). "(1355) Magoeba". Dictionary of Minor Planet Names – (1355) Magoeba. Springer Berlin Heidelberg. p. 110. doi:10.1007/978-3-540-29925-7_1356. ISBN   978-3-540-00238-3.
    3. 1 2 3 "1355 Magoeba (1935 HE)". Minor Planet Center. Retrieved 13 January 2017.
    4. 1 2 3 4 5 6 "LCDB Data for (1355) Magoeba". Asteroid Lightcurve Database (LCDB). Retrieved 13 January 2017.
    5. 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 . Retrieved 13 January 2017.
    6. 1 2 3 4 5 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.
    7. 1 2 3 Warner, Brian D. (January 2015). "A Sextet of Main-belt Binary Asteroid Candidates". The Minor Planet Bulletin. 42 (1): 60–66. Bibcode:2015MPBu...42...60W. ISSN   1052-8091 . Retrieved 13 January 2017.
    8. 1 2 Warner, Brian D. (October 2013). "Asteroid Lightcurve Analysis at CS3-Palmer Divide Station: 2013 May-June". The Minor Planet Bulletin. 40 (4): 208–212. Bibcode:2013MPBu...40..208W. ISSN   1052-8091 . Retrieved 13 January 2017.
    9. 1 2 3 Warner, Brian D. (April 2010). "Asteroid Lightcurve Analysis at the Palmer Divide Observatory: 2009 September-December". The Minor Planet Bulletin. 37 (2): 57–64. Bibcode:2010MPBu...37...57W. ISSN   1052-8091 . Retrieved 13 January 2017.
    10. 1 2 Warner, Brian D. (October 2011). "Asteroid Lightcurve Analysis at the Palmer Divide Observatory: 2011 March - July". The Minor Planet Bulletin. 38 (4): 190–195. Bibcode:2011MPBu...38..190W. ISSN   1052-8091 . Retrieved 13 January 2017.
    11. 1 2 Warner, Brian D. (March 2007). "Asteroid Lightcurve Analysis at the Palmer Divide Observatory - June-September 2006". The Minor Planet Bulletin. 34 (1): 8–10. Bibcode:2007MPBu...34....8W. ISSN   1052-8091 . Retrieved 13 January 2017.
    12. 1 2 Gil-Hutton, R.; Lazzaro, D.; Benavidez, P. (June 2007). "Polarimetric observations of Hungaria asteroids". Astronomy and Astrophysics. 468 (3): 1109–1114. Bibcode:2007A&A...468.1109G. doi: 10.1051/0004-6361:20077178 . hdl: 11336/213855 . Retrieved 13 January 2017.
    13. 1 2 3 Fornasier, S.; Clark, B. E.; Dotto, E. (July 2011). "Spectroscopic survey of X-type asteroids". Icarus. 214 (1): 131–146. arXiv: 1105.3380 . Bibcode:2011Icar..214..131F. doi:10.1016/j.icarus.2011.04.022 . Retrieved 13 January 2017.
    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 13 January 2017.
    15. ↑ Schmadel, Lutz D. "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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