1226 Golia

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1226 Golia
001226-asteroid shape model (1226) Golia.png
Shape model of Golia from its lightcurve
Discovery [1]
Discovered by H. van Gent
Discovery site Johannesburg Obs.
(Leiden Southern Station)
Discovery date22 April 1930
Designations
(1226) Golia
Named after
 Jacobus Golius
(Dutch mathematician) [2]
1930 HL ·1957 WN
main-belt  ·(middle) [3]
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc 87.20 yr (31,851 days)
Aphelion 2.8736 AU
Perihelion 2.2927 AU
2.5832 AU
Eccentricity 0.1124
4.15 yr (1,516 days)
57.385°
0° 14m 14.64s / day
Inclination 9.8470°
17.486°
139.78°
Physical characteristics
Dimensions11.679±0.158 km [4]
12.179±0.147 km [5]
15.92 km (derived) [3]
16.39±1.5 km [6]
4.0910±0.0005 h [7]
4.097 h [8]
0.1008 (derived) [3]
0.1724±0.0240 [5]
0.187±0.023 [4]
0.2388±0.052 [6]
M [5]  · S [3]
11.10 [6]  ·11.809±0.003(R) [7]  ·12.1 [3] [5]  ·12.2 [1]  ·12.39±0.61 [9]

    1226 Golia, provisional designation 1930 HL, is a metallic asteroid from the central region of the asteroid belt, approximately 15 kilometers in diameter. It was discovered on 22 April 1930, by Dutch astronomer Hendrik van Gent at Leiden Southern Station, annex to the Johannesburg Observatory in South Africa. [10] It is named for Jacobus Golius. [2]

    Contents

    Orbit and classification

    Golia orbits the Sun in the central main-belt at a distance of 2.3–2.9  AU once every 4 years and 2 months (1,516 days). Its orbit has an eccentricity of 0.11 and an inclination of 10° with respect to the ecliptic. [1] The body's observation arc begins at Johannesburg one night after its official discovery observation, with no precoveries taken and no prior identifications made. [10]

    Physical characteristics

    Golia has been characterized as a metallic M-type asteroid by the Wide-field Infrared Survey Explorer (WISE). [5]

    Rotation period

    In March 1992, the first reliable rotational light curve of Golia was obtained by Italian astronomer Mario Di Martino using the ESO 1-metre telescope at La Silla in northern Chile. Analysis gave a well-defined rotation period of 4.097 hours with a change in brightness of 0.35 magnitude ( U=3 ). [8] Another light curve was obtained from photometric observations in the R-band at the Palomar Transient Factory in October 2011, giving a period of 4.0910 hours and an amplitude of 0.24 magnitude ( U=2 ). [7]

    Diameter and albedo

    According to preliminary results by the NEOWISE mission of NASA's WISE space telescope, Golia measures 11.68 and 12.18 kilometers in diameter, and its surface has an albedo of 0.187 and 0.172, respectively, [4] [5] while the Infrared Astronomical Satellite IRAS gives a diameter of 16.39 kilometers and an albedo of 0.239. [6] The Collaborative Asteroid Lightcurve Link considers Golia to be of stony composition, deriving an albedo of 0.1008 and a diameter of 15.92 kilometers, using an absolute magnitude of 12.1. [3]

    Naming

    This minor planet was named after Dutch professor of astronomy Jakob Gool (1596–1667), also known as Jacobus Golius, who founded the Leiden Observatory in 1633. He was a mathematician and orientalist, who translated Arabic texts into Latin including the work of 9th-century Muslim astronomer Al-Farghani. He was also a teacher of French philosopher René Descartes, after whom the minor planet 3587 Descartes is named. [2] The official naming citation was compiled by Lutz Schmadel for the Dictionary of Minor Planet Names based on a private communication with Ingrid van Houten-Groeneveld at Leiden. [2]

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    References

    1. 1 2 3 4 "JPL Small-Body Database Browser: 1226 Golia (1930 HL)" (2017-07-05 last obs.). Jet Propulsion Laboratory . Retrieved 26 July 2017.
    2. 1 2 3 4 Schmadel, Lutz D. (2007). "(1226) Golia". Dictionary of Minor Planet Names – (1226) Golia. Springer Berlin Heidelberg. p. 102. doi:10.1007/978-3-540-29925-7_1227. ISBN   978-3-540-00238-3.
    3. 1 2 3 4 5 6 "LCDB Data for (1226) Golia". Asteroid Lightcurve Database (LCDB). Retrieved 26 January 2017.
    4. 1 2 3 Masiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Dailey, J.; et al. (November 2011). "Main Belt Asteroids with WISE/NEOWISE. I. Preliminary Albedos and Diameters". The Astrophysical Journal. 741 (2): 20. arXiv: 1109.4096 . Bibcode:2011ApJ...741...68M. doi:10.1088/0004-637X/741/2/68 . Retrieved 26 January 2017.
    5. 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.
    6. 1 2 3 4 Tedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (October 2004). "IRAS Minor Planet Survey V6.0". NASA Planetary Data System. 12: IRAS-A-FPA-3-RDR-IMPS-V6.0. Bibcode:2004PDSS...12.....T . Retrieved 22 October 2019.
    7. 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 26 January 2017.
    8. 1 2 di Martino, Mario; Dotto, E.; Barucci, M. A.; Fulchignoni, M.; Rotundi, A. (May 1994). "Photoelectric photometry of ten small and fast spinning asteroids". Icarus. 109 (1): 210–218. Bibcode:1994Icar..109..210D. doi:10.1006/icar.1994.1087. ISSN   0019-1035. Archived from the original on 2 February 2017. Retrieved 26 January 2017.
    9. ↑ 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 26 January 2017.
    10. 1 2 "1226 Golia (1930 HL)". Minor Planet Center. Retrieved 26 January 2017.
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