1142 Aetolia

1142 Aetolia, provisional designation 1930 BC, is a stony background asteroid from the outer region of the asteroid belt, approximately 24 kilometers in diameter. It was discovered on 24 January 1930, by German astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory and named for the Greek region Aetolia.[3][12]

1142 Aetolia
Discovery [1]
Discovered byK. Reinmuth
Discovery siteHeidelberg Obs.
Discovery date24 January 1930
Designations
(1142) Aetolia
Pronunciation/iːˈtoʊliə/[2]
Named after
Aetolia (Greek region)[3]
1930 BC · 1931 LC
1937 LN · 1937 LU
1942 GF · 1942 GS
1943 PF · 1948 JS
1948 KG · 1954 KJ
1954 MU · 1958 BB
A902 GB · A907 CB
A908 GB
main-belt · (outer) [4]
Orbital characteristics [1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc115.24 yr (42,093 days)
Aphelion3.4423 AU
Perihelion2.9265 AU
3.1844 AU
Eccentricity0.0810
5.68 yr (2,076 days)
90.209°
0° 10m 24.24s / day
Inclination2.1096°
139.34°
96.492°
Physical characteristics
Dimensions22.135±0.133 km[5]
23.764±0.124 km[6]
24.92±1.57 km[7]
27.10 km (calculated)[4]
7.68±0.12 h[8]
10.730±0.005 h[9]
10.74±0.02 h[10]
0.20 (assumed)[4]
0.216±0.029[7]
0.2439±0.0610[6]
0.273±0.034[5]
S [4][11]
9.95±0.07 (R)[8] · 10.2[1][4] · 10.30[6][7] · 10.35±0.29[11]

    Orbit and classification

    Aetolia has not been associated with any known asteroid family. It orbits the Sun in the outer main-belt at a distance of 2.9–3.4 AU once every 5 years and 8 months (2,076 days). Its orbit has an eccentricity of 0.08 and an inclination of 2° with respect to the ecliptic.[1]

    The asteroid was first identified as A902 GB at Heidelberg in April 1902. The body's observation arc begins at the USNO in May 1908, or 22 years prior to its official discovery observation.[12]

    Physical characteristics

    Aetolia has been characterized as a common stony S-type asteroid by Pan-STARRS photometric survey.[11]

    Rotation period

    In May 2010, two rotational lightcurves of Aetolia were independently obtained from photometric observations by French amateur astronomer René Roy and by Russell Durkee at the S.O.S. Observatory (H39) near Minneapolis, United States. Lightcurve analysis gave a rotation period of 10.730 and 10.74 hours with a brightness variation of 0.20 and 0.22 in magnitude, respectively (U=3-/3-).[9][10] A more recent and lower-rated observation gave a divergent period of 7.68 hours (U=2).[8]

    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, Aetolia measures between 22.135 and 24.92 kilometers in diameter and its surface has an albedo between 0.216 and 0.273.[5][6][7]

    The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 27.10 kilometers based on an absolute magnitude of 10.2.[4]

    Naming

    This minor planet was named after the Greek region Aetolia, north of the Gulf of Patras. The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 107).[3]

    References
    1. "JPL Small-Body Database Browser: 1142 Aetolia (1930 BC)" (2017-07-05 last obs.). Jet Propulsion Laboratory. Retrieved 25 August 2017.
    2. "Aetolia". Merriam-Webster Dictionary.
    3. Schmadel, Lutz D. (2007). "(1142) Aetolia". Dictionary of Minor Planet Names – (1142) Aetolia. Springer Berlin Heidelberg. p. 97. doi:10.1007/978-3-540-29925-7_1143. ISBN 978-3-540-00238-3.
    4. "LCDB Data for (1142) Aetolia". Asteroid Lightcurve Database (LCDB). Retrieved 25 August 2017.
    5. 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 25 August 2017.
    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. 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. Retrieved 17 October 2019. (online, AcuA catalog p. 153)
    8. Chang, Chan-Kao; Lin, Hsing-Wen; Ip, Wing-Huen; Prince, Thomas A.; Kulkarni, Shrinivas R.; Levitan, David; et al. (December 2016). "Large Super-fast Rotator Hunting Using the Intermediate Palomar Transient Factory". The Astrophysical Journal Supplement Series. 227 (2): 13. arXiv:1608.07910. Bibcode:2016ApJS..227...20C. doi:10.3847/0067-0049/227/2/20. Retrieved 25 August 2017.
    9. Durkee, Russell I. (January 2011). "Asteroids Observed from the Shed of Science Observatory: 2010 May-October". The Minor Planet Bulletin. 38 (1): 39–40. Bibcode:2011MPBu...38...39D. ISSN 1052-8091. Retrieved 25 August 2017.
    10. Behrend, Raoul. "Asteroids and comets rotation curves – (1142) Aetolia". Geneva Observatory. Retrieved 25 August 2017.
    11. 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 25 August 2017.
    12. "1142 Aetolia (1930 BC)". Minor Planet Center. Retrieved 25 August 2017.

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