812 Adele

812 Adele (prov. designation: A915 RU or 1915 XV) is an elongated Eunomia asteroid from the central regions of the asteroid belt. It was discovered on 8 September 1915, by Russian astronomer Sergey Belyavsky at the Simeiz Observatory on the Crimean peninsula.[1] The presumed S-type asteroid has a rotation period of 5.9 hours and measures approximately 13 kilometers (8 miles) in diameter. It was likely named after the character "Adele" in the opera Die Fledermaus by Johann Strauss.[2]

812 Adele
Modelled shape of Adele from its lightcurve
Discovery [1]
Discovered byS. Belyavskyj
Discovery siteSimeiz Obs.
Discovery date8 September 1915
Designations
(812) Adele
Named after
Adele, character in the operetta Die Fledermaus [2]
A915 RU · A902 UE
1915 XV
Orbital characteristics [3]
Epoch 31 May 2020 (JD 2459000.5)
Uncertainty parameter 0
Observation arc104.40 yr (38,132 d)
Aphelion3.0981 AU
Perihelion2.2220 AU
2.6601 AU
Eccentricity0.1647
4.34 yr (1,585 d)
46.769°
0° 13m 37.92s / day
Inclination13.298°
7.2582°
353.10°
Physical characteristics
Mean diameter
5.8587±0.0002 h[9]
  • (301.0°, 44.0°) (λ1/β1)[5]
  • (154.0°, 69.0°) (λ2/β2)[5]
  • 0.257±0.019[8]
  • 0.291±0.041[7]
S (family-based)[10][11]

    Orbit and classification

    When applying the hierarchical clustering method to its proper orbital elements, Adele is a core member of the Eunomia family (502),[4][5][6] a prominent family of stony S-type asteroids and the largest one in the intermediate main belt with more than 5,000 known members.[11]: 23  It orbits the Sun in the central asteroid belt at a distance of 2.2–3.1 AU once every 4 years and 4 months (1,585 days; semi-major axis of 2.66 AU). Its orbit has an eccentricity of 0.16 and an inclination of 13° with respect to the ecliptic.[3]

    Discovery

    Adele was discovered by Russian astronomer Sergey Belyavsky at the Simeiz Observatory on the Crimean peninsula 8 September 1915. Three nights later, on 11 September 1915, it was independently discovered by Max Wolf the Heidelberg Observatory in Germany. The Minor Planet Center however, only credits the first discoverer. The asteroid was first observed as A902 UE at Heidelberg on 25 October 1902. The body's observation arc begins at the Bergedorf Observatory on 19 September 1915, less than two weeks after its official discovery observation.[1]

    Naming

    This minor planet was likely named after "Adele", Rosalinde's maid, a character in the operetta Die Fledermaus by Johann Strauss (1825–1899). The name was given by the independent discoverer Max Wolf. The author of the Dictionary of Minor Planet Names, Lutz Schmadel, learned about the meaning of the asteroid's name from R. Bremer and Ingrid van Houten-Groeneveld, latter who worked as a young astronomer at Heidelberg.

    Physical characteristics

    Based on the overall spectral type of the Eunomia family,[11]: 23  Adele is likely a common, stony S-type asteroid.[10]

    Lightcurve-based 3D-model of Adele

    Rotation period

    In October 2002, a rotational lightcurve of Adele was obtained from photometric observations by French amateur astronomer René Roy. Lightcurve analysis gave a well-defined rotation period of 5.8587±0.0002 hours with a high brightness variation of 0.69±0.02 magnitude, indicative of an elongated shape (U=3).[9]

    In 2016, a modeled lightcurve gave a concurring sidereal period of 5.85746±0.00002 hours using data from the Uppsala Asteroid Photometric Catalogue, the Palomar Transient Factory survey, and individual observers (such as above), as well as sparse-in-time photometry from the NOFS, the Catalina Sky Survey, and the La Palma surveys (950). The study also determined two spin axes at (301.0°, 44.0°) and (154.0°, 69.0°) in ecliptic coordinates (λ, β).[12]

    Diameter and albedo

    According to the surveys carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE) and the Japanese Akari satellite, Adele measures (12.356±0.111) and (13.57±0.43) kilometers in diameter and its surface has an albedo of (0.291±0.041) and (0.257±0.019), respectively.[7][8] The Collaborative Asteroid Lightcurve Link assumes a standard albedo for a Eunomian asteroid of 0.21 and calculates a diameter of 12.66 kilometers based on an absolute magnitude of 11.8.[10] Alternative mean-diameter measurements published by the WISE team include (11.93±0.33 km) and (13.619±0.263 km) with corresponding albedos of (0.259±0.047) and (0.2420±0.0275).[5][10]

    References
    1. "812 Adele (A915 RU)". Minor Planet Center. Retrieved 25 March 2020.
    2. Schmadel, Lutz D. (2007). "(812) Adele". Dictionary of Minor Planet Names. Springer Berlin Heidelberg. p. 75. doi:10.1007/978-3-540-29925-7_813. ISBN 978-3-540-00238-3.
    3. "JPL Small-Body Database Browser: 812 Adele (A915 RU)" (2020-02-04 last obs.). Jet Propulsion Laboratory. Retrieved 25 March 2020.
    4. "Asteroid 812 Adele – Proper Elements". AstDyS-2, Asteroids – Dynamic Site. Retrieved 25 March 2020.
    5. "Asteroid 812 Adele – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 25 March 2020.
    6. Zappalà, V.; Bendjoya, Ph.; Cellino, A.; Farinella, P.; Froeschle, C. (1997). "Asteroid Dynamical Families". NASA Planetary Data System: EAR-A-5-DDR-FAMILY-V4.1. Retrieved 25 March 2020.} (PDS main page)
    7. Mainzer, A. K.; Bauer, J. M.; Cutri, R. M.; Grav, T.; Kramer, E. A.; Masiero, J. R.; et al. (June 2016). "NEOWISE Diameters and Albedos V1.0". NASA Planetary Data System: EAR-A-COMPIL-5-NEOWISEDIAM-V1.0. Bibcode:2016PDSS..247.....M. Retrieved 25 March 2020.
    8. 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. (online, AcuA catalog p. 153)
    9. Behrend, Raoul. "Asteroids and comets rotation curves – (812) Adele". Geneva Observatory. Retrieved 25 March 2020.
    10. "LCDB Data for (812) Adele". Asteroid Lightcurve Database (LCDB). Retrieved 25 March 2020.
    11. Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families". Asteroids IV. pp. 297–321. arXiv:1502.01628. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. ISBN 9780816532131.
    12. Hanuš, J.; Ďurech, J.; Brož, M.; Marciniak, A.; Warner, B. D.; Pilcher, F.; et al. (March 2013). "Asteroids' physical models from combined dense and sparse photometry and scaling of the YORP effect by the observed obliquity distribution". Astronomy and Astrophysics. 551: A67. arXiv:1301.6943. Bibcode:2013A&A...551A..67H. doi:10.1051/0004-6361/201220701. ISSN 0004-6361.
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