1027 Aesculapia

1027 Aesculapia, provisional designation A923 YO11, is a Themistian asteroid from the outer region of the asteroid belt, approximately 33 kilometers in diameter.

1027 Aesculapia
Discovery [1]
Discovered byG. van Biesbroeck
Discovery siteYerkes Obs.
Discovery date11 November 1923
Designations
(1027) Aesculapia
Pronunciation/ɛskjʊˈleɪpiə/[2]
Named after
Aesculāpius
(Greek/Roman deity)[3]
A923 YO11 · 1942 DH
1977 LP1 · A899 PE
A908 AE
main-belt · Themis [4]
Orbital characteristics [1]
Epoch 16 February 2017 (JD 2457800.5)
Uncertainty parameter 0
Observation arc108.41 yr (39,595 days)
Aphelion3.5625 AU
Perihelion2.7408 AU
3.1517 AU
Eccentricity0.1304
5.60 yr (2,044 days)
121.70°
0° 10m 34.32s / day
Inclination1.2537°
29.346°
132.13°
Physical characteristics
Dimensions31.225±0.164 km[5]
32.05 km (derived)[4]
32.20±1.4 km[6]
32.38±8.42 km[7]
34.464±0.335 km[8]
35.25±13.39 km[9]
38.55±0.82 km[10]
6.83±0.10 h (incorrect)[11]
9.791±0.002 h[12]
10 h (fragmentary)[13]
13.529±0.042 h[lower-alpha 1]
19.506±0.1501 h[14]
0.06±0.08[9]
0.07±0.05[7]
0.071±0.003[10]
0.0750 (derived)[4]
0.0856±0.0056[8]
0.0981±0.009[6]
0.129±0.014[5]
S [4]
10.6[6][8][10] · 10.80[9] · 10.9[1][4] · 10.95[7] · 11.089±0.001 (S)[14]

    It was discovered on 11 November 1923, by Belgian–American astronomer George Van Biesbroeck at Yerkes Observatory in Williams Bay, Wisconsin, United States.[15] It is named for Aesculapius, the god of medicine in Greek mythology.[3]

    Classification and orbit

    Aesculapia is a member of the Themis family, a dynamical group of carbonaceous outer-belt asteroids which are known for their nearly coplanar ecliptical orbits. It orbits the Sun at a distance of 2.7–3.6 AU once every 5 years and 7 months (2,044 days). Its orbit has an eccentricity of 0.13 and an inclination of 1° with respect to the ecliptic.[1]

    In 1889, it was first identified as A899 PE at Harvard Observatory's Boyden Station in Arequipa, Peru. The body's observation arc begins at Heidelberg in 1908, when it was identified as A908 AE, 15 years prior to its official discovery observation at Williams Bay.[15]

    Diameter and albedo

    According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite, and NASA's Wide-field Infrared Survey Explorer with its subsequent NEOWISE mission, Aesculapia measures between 31.225 and 38.55 kilometers in diameter, and its surface has an albedo between and 0.06 and 0.129.[5][6][7][8][9][10]

    The Collaborative Asteroid Lightcurve Link (CALL) derives an albedo of 0.075 and a diameter of 32.05 kilometers with an absolute magnitude of 10.9.[4] Despite the body's low albedo, CALL classifies Aesculapia as a S-type rather than a C-type asteroid.[4]

    Photometry

    In the last 20 years, photometric observations of Aesculapia gave several rotational lightcurves with significantly divergent rotation periods. First results obtained by Chester Maleszewski and René Roy were only fragmentary or incorrect (U=1/1).[11][13] Photometry at the Palomar Transient Factory and observations by Astronomer Steven Ehlert gave a period of 9.791 and 19.506 hours with a brightness amplitude of 0.09 and 0.19 magnitude, respectively (U=2/2).[12][14] CALL currently adopts a lightcurve obtained by Kylie Hess at Oakley Southern Sky Observatory in March 2015, which gave a period of 13.529 hours and a brightness variation of 0.09 magnitude (U=2).[lower-alpha 1]

    Naming

    This minor planet was named for Aesculapius, the Greek and Roman demigod of medicine and healing, son of Apollo and Coronis, after whom the asteroids 158 Koronis and 1862 Apollo are named, respectively.[3] Naming citation was first mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 98).[3]

    Notes
    1. Hess (2017) : rotation period 13.529±0.042 hours with a brightness amplitude of 0.09 mag and Quality Code of 2. Summary figures at Collaborative Asteroid Lightcurve Link (CALL) for (1027) Aesculapia; to be available at ADS Bibcode:[https://ui.adsabs.harvard.edu/abs/20167PBu...44....3H/abstract 20167PBu...44....3HCheck bibcode: value (help)]

    References
    1. "JPL Small-Body Database Browser: 1027 Aesculapia (A923 YO11)" (2016-06-09 last obs.). Jet Propulsion Laboratory. Retrieved 8 February 2017.
    2. "Æsculapius". Oxford English Dictionary (Online ed.). Oxford University Press. (Subscription or participating institution membership required.)
    3. Schmadel, Lutz D. (2007). "(1027) Aesculapia". Dictionary of Minor Planet Names – (1027) Aesculapia. Springer Berlin Heidelberg. p. 88. doi:10.1007/978-3-540-29925-7_1028. ISBN 978-3-540-00238-3.
    4. "LCDB Data for (1027) Aesculapia". Asteroid Lightcurve Database (LCDB). Retrieved 8 February 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 8 February 2017.
    6. 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. Nugent, C. R.; Mainzer, A.; Bauer, J.; Cutri, R. M.; Kramer, E. A.; Grav, T.; et al. (September 2016). "NEOWISE Reactivation Mission Year Two: Asteroid Diameters and Albedos". The Astronomical Journal. 152 (3): 12. arXiv:1606.08923. Bibcode:2016AJ....152...63N. doi:10.3847/0004-6256/152/3/63. Retrieved 8 February 2017.
    8. 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.
    9. Nugent, C. R.; Mainzer, A.; Masiero, J.; Bauer, J.; Cutri, R. M.; Grav, T.; et al. (December 2015). "NEOWISE Reactivation Mission Year One: Preliminary Asteroid Diameters and Albedos". The Astrophysical Journal. 814 (2): 13. arXiv:1509.02522. Bibcode:2015ApJ...814..117N. doi:10.1088/0004-637X/814/2/117. Retrieved 8 February 2017.
    10. 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)
    11. Maleszewski, Chester; Clark, Maurice (December 2004). "Bucknell University Observatory lightcurve results for 2003-2004". The Minor Planet Bulletin. 31 (4): 93–94. Bibcode:2004MPBu...31...93M. ISSN 1052-8091. Retrieved 8 February 2017.
    12. Ehlert, Steven; Kingery, Aaron (July 2015). "New Lightcurves of 1027 Aesculapia and 3395 Jitka". The Minor Planet Bulletin. 42 (3): 211. Bibcode:2015MPBu...42..211E. ISSN 1052-8091. Retrieved 8 February 2017.
    13. Behrend, Raoul. "Asteroids and comets rotation curves – (1027) Aesculapia". Geneva Observatory. Retrieved 8 February 2017.
    14. 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 8 February 2017.
    15. "1027 Aesculapia (A923 YO11)". Minor Planet Center. Retrieved 8 February 2017.

    This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.