1027 Aesculapia

Last updated

1027 Aesculapia
Discovery [1]
Discovered by G. van Biesbroeck
Discovery site Yerkes 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 arc 108.41 yr (39,595 days)
Aphelion 3.5625 AU
Perihelion 2.7408 AU
3.1517 AU
Eccentricity 0.1304
5.60 yr (2,044 days)
121.70°
0° 10m 34.32s / day
Inclination 1.2537°
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]

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

    Contents

    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. 1 2 Hess (2017): [lower-alpha 2] 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

    Related Research Articles

    <span class="mw-page-title-main">2829 Bobhope</span> Dark asteroid of the Meliboea family

    2829 Bobhope is a dark asteroid of the Meliboea family, from the outer region of the asteroid belt. It was discovered on 9 August 1948, by South African astronomer Ernest Leonard Johnson at Union Observatory in Johannesburg. The asteroid was later named after comedian Bob Hope. The asteroid has a rotation period of 6.1 hours and measures approximately 37 kilometers in diameter.

    1024 Hale, provisional designation A923 YO13, is a carbonaceous background asteroid from the outer regions of the asteroid belt, approximately 45 kilometers (28 miles) in diameter. The asteroid was discovered on 2 December 1923, by Belgian–American astronomer George Van Biesbroeck at the Yerkes Observatory in Wisconsin, United States. It was named for American astronomer George Ellery Hale. The dark C-type asteroid may have a rotation period of 16 hours.

    1178 Irmela, provisional designation 1931 EC, is a stony asteroid from the middle regions of the asteroid belt, approximately 19 kilometers in diameter.

    1049 Gotho, provisional designation 1925 RB, is a carbonaceous asteroid from the outer region of the asteroid belt, approximately 53 kilometers in diameter. It was discovered on 14 September 1925, by German astronomer Karl Reinmuth at Heidelberg Observatory in southwest Germany. Although the name of the asteroid is a masculine German name, it is not known to refer to a particular individual.

    1096 Reunerta, provisional designation 1928 OB, is an asteroid from the background population of the asteroid belt's central region, approximately 40 kilometers in diameter. It was discovered on 21 July 1928, by astronomer Harry Edwin Wood at the Union Observatory in Johannesburg, South Africa. The asteroid was named after South African engineer Theodore Reunert, supporter of the observatory and friend of the discoverer.

    <span class="mw-page-title-main">1554 Yugoslavia</span> Stony Eunomian asteroid from the middle region of the asteroid belt

    1554 Yugoslavia, provisional designation 1940 RE, is a stony Eunomian asteroid from the middle region of the asteroid belt, approximately 16 kilometres (9.9 mi) in diameter. It was discovered by Serbian astronomer Milorad Protić at Belgrade Astronomical Observatory, Serbia, on 6 September 1940. It was named for the former country of Yugoslavia.

    <span class="mw-page-title-main">1127 Mimi</span>

    1127 Mimi is a dark background asteroid from the central regions of the asteroid belt. It was discovered on 13 January 1929, by Belgian astronomer Sylvain Arend at the Royal Observatory of Belgium in Uccle. The carbonaceous C-type asteroids (CX) has a rotation period of 12.7 hours and measures approximately 47 kilometers in diameter. Through a glitch in the naming process, the asteroid received the name "Mimi" instead of "Robelmonte" as originally intended by the discoverer.

    <span class="mw-page-title-main">1165 Imprinetta</span> Carbonaceous Meliboean asteroid

    1165 Imprinetta, provisional designation 1930 HM, is a carbonaceous Meliboean asteroid from the outer regions of the asteroid belt, approximately 49 kilometers (30 mi) in diameter. It was discovered on 24 April 1930 by Dutch astronomer Hendrik van Gent at the Union Observatory in Johannesburg, South Africa. The asteroid was named after Imprinetta Gent, wife of the discoverer.

    1194 Aletta, provisional designation 1931 JG, is a carbonaceous asteroid from the outer region of the asteroid belt, approximately 55 kilometers in diameter. It was discovered on 13 May 1931, by South African astronomer Cyril Jackson at Johannesburg Observatory in South Africa. It was later named after the discoverer's wife Aletta Jackson.

    11277 Ballard (provisional designation 1988 TW2) is a Phocaea asteroid from the inner regions of the asteroid belt, approximately 6.3 kilometers (3.9 miles) in diameter. It was discovered on 8 October 1988, by American astronomer couple Carolyn and Eugene Shoemaker at the Palomar Observatory in California. The assumed S-type asteroid has a rotation period of at least 10 hours. It was named for American marine scientist Robert Ballard.

    1815 Beethoven, provisional designation 1932 CE1, is a carbonaceous background asteroid from the outer regions of the asteroid belt, approximately 30 kilometers (19 miles) in diameter. It was discovered on 27 January 1932, by German astronomer Karl Reinmuth at the Heidelberg Observatory. The uncommon F-type asteroid seems to have a long rotation period of 54 hours (tentative). It was named after Ludwig van Beethoven.

    2038 Bistro, provisional designation 1973 WF, is a stony asteroid from the inner regions of the asteroid belt, approximately 12 kilometers in diameter. The asteroid was discovered on 24 November 1973, by Swiss astronomer Paul Wild at the Zimmerwald Observatory near Bern, Switzerland. It was named for the Bistro restaurant.

    2008 Konstitutsiya, provisionally designated 1973 SV4, is a carbonaceous asteroid from the outer region of the asteroid belt, approximately 50 kilometers in diameter. It was discovered on 27 September 1973, by Soviet astronomer Lyudmila Chernykh at the Crimean Astrophysical Observatory in Nauchnyj, on the Crimean peninsula. The asteroid was named for the 1977 Soviet Constitution.

    1284 Latvia, provisional designation 1933 OP, is a rare-type asteroid from the middle region of the asteroid belt, approximately 37 kilometers in diameter. It was discovered on 27 July 1933, by German astronomer Karl Reinmuth at Heidelberg Observatory in southern Germany, and named after the Republic of Latvia.

    1383 Limburgia, provisional designation 1934 RV, is a carbonaceous asteroid from the outer region of the asteroid belt, approximately 23 kilometers in diameter. It was discovered on 9 September 1934, by Dutch astronomer Hendrik van Gent at the Leiden Southern Station, annex to the Johannesburg Observatory in South Africa. It is named for the Dutch province Limburg.

    1359 Prieska, provisional designation 1935 OC, is a rare-type carbonaceous asteroid from the outer region of the asteroid belt, approximately 50 kilometers in diameter. It was discovered on 22 July 1935, by English-born South-African astronomer Cyril Jackson at Johannesburg Observatory in South Africa. The asteroid was named after the South African town of Prieska.

    1258 Sicilia, provisional designation 1932 PG, is a dark background asteroid from the outer regions of the asteroid belt, approximately 44 kilometers in diameter. It was discovered on 8 August 1932, by astronomer Karl Reinmuth at the Heidelberg-Königstuhl State Observatory in southwest Germany. The asteroid was named after the Italian island of Sicily.

    1330 Spiridonia, provisional designation 1925 DB, is a dark background asteroid of primitive composition, located in the outer regions of the asteroid belt, approximately 65 kilometers in diameter. It was discovered on 17 February 1925, by Soviet astronomer Vladimir Albitsky at the Simeiz Observatory on the Crimean peninsula. The asteroid was named after the discoverer's brother-in-law, Spiridon Zaslavskij.

    1266 Tone is a dark background asteroid from the outer regions of the asteroid belt, approximately 80 kilometers in diameter. Discovered by astronomer Okuro Oikawa at the Tokyo Observatory in 1927, it was assigned the provisional designation 1927 BD. The asteroid was later named after the Tone River, one of Japan's largest rivers.

    3682 Welther, provisional designation A923 NB, is a background asteroid from the central regions of the asteroid belt, approximately 19 kilometers in diameter. It was discovered on 12 July 1923, by German astronomer Karl Reinmuth at the Heidelberg Observatory in southwest Germany. The asteroid has a rotation period of 3.6 hours. It was named after Barbara Welther, an American historian of science at CfA.

    References

    1. 1 2 3 4 "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. 1 2 3 4 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. 1 2 3 4 5 6 7 "LCDB Data for (1027) Aesculapia". Asteroid Lightcurve Database (LCDB). Retrieved 8 February 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. S2CID   119293330 . Retrieved 8 February 2017.
    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 4 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 .
    8. 1 2 3 4 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. S2CID   35447010.
    9. 1 2 3 4 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. S2CID   9341381 . Retrieved 8 February 2017.
    10. 1 2 3 4 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)
    11. 1 2 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. 1 2 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. 1 2 Behrend, Raoul. "Asteroids and comets rotation curves – (1027) Aesculapia". Geneva Observatory . Retrieved 8 February 2017.
    14. 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. S2CID   8342929 . Retrieved 8 February 2017.
    15. 1 2 "1027 Aesculapia (A923 YO11)". Minor Planet Center. Retrieved 8 February 2017.
    16. Hess, Kylie; Bruner, Madison; Ditteon, Richard (January 2017). "The Minor Planet Bulletin: Asteroid Lightcurve Analysis at the Oakley Southern Sky Observatory: 2015 February–March". Bulletin of the Minor Planets Section of the Association of Lunar and Planetary Observers. 44 (1): 3–4. Bibcode:2017MPBu...44....3H. ISSN   1052-8091.
    This page is based on this Wikipedia article
    Text is available under the CC BY-SA 4.0 license; additional terms may apply.
    Images, videos and audio are available under their respective licenses.