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1509 Esclangona

From Wikipedia, the free encyclopedia
Hungaria asteroid and binary system from the inner regions of the asteroid belt

1509 Esclangona
Discovery[1]
Discovered byA. Patry
Discovery siteNice Obs.
Discovery date21 December 1938
Designations
(1509) Esclangona
Named after
Ernest Esclangon
(French astronomer)[2]
1938 YG
main-belt · (inner)[1]
Hungaria[3][4][5]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc77.68 yr (28,374 days)
Aphelion1.9263AU
Perihelion1.8064 AU
1.8663 AU
Eccentricity0.0321
2.55yr (931 days)
225.08°
0° 23m 11.76s / day
Inclination22.320°
283.52°
267.82°
Knownsatellites1[6]
Physical characteristics
Dimensions6.83±1.32 km[7]
7.52±1.78 km[8]
8.17±0.6 km(IRAS:2)[9]
8.18 km(derived)[4]
9.0±1.0 km[10]
9.87±0.37 km[11]
2.64±0.02 h[12]
3.247 h[10]
3.247±0.002 h[13]
3.252±0.005 h[14][a]
3.2524±0.0003 h[15]
3.25250±0.00005 h[16]
3.25281±0.00002 h[b]
3.25283±0.00002 h[17]
5.89h[c]
0.107±0.021[10]
0.160±0.013[11]
0.185±0.055[18]
0.2041(derived)[4]
0.2327±0.038(IRAS:2)[9]
0.30±0.14[8]
0.41±0.18[7]
Tholen =S[1] · K[19] · S[4]
B–V = 0.894[1]
U–B = 0.472[1]
12.33±0.14(R)[b] · 12.64[1][7][9][11] · 12.79[8] · 12.858±0.149[4][20] · 13.28±0.0[10]

1509 Esclangona (provisional designation1938 YG) is a rare-type Hungariaasteroid andbinary system from the inner regions of theasteroid belt, approximately 8 kilometers in diameter. It is named after French astronomerErnest Esclangon.

Discoveries

[edit]

Esclangona was discovered on 21 December 1938, by French astronomerAndré Patry atNice Observatory. The body'sobservation arc begins with its official discovery observation as noprecoveries were taken, and no prior identifications were made.[3] On 13 February 2003, aminor-planet moon in orbit of Esclangona was discovered by astronomers at ESO'sVery Large Telescope (UT4) onCerro Paranal in Chile.[2][3]

Orbit and classification

[edit]

Esclangona is a member of theHungaria family, which form the innermost concentration of asteroids in theSolar System. It orbits the Sun in theinner main-belt at a distance of 1.8–1.9 AU once every 2 years and 7 months (931 days). Its orbit has aneccentricity of 0.03 and aninclination of 22° with respect to theecliptic.[1]

Binary system

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Esclangona has a smallmoon, provisionally designatedS/2003 (1509) 1, which measures 4 kilometers in diameter, and orbits 140 kilometers from its parent. This wide separation relative to the pair's size is rather unusual and it is believed that both Esclangona and its moon areejecta from an asteroidal collision in the past that left the scene as a co-orbiting pair; a similar pairing is3749 Balam and its outer moon.[6]

Physical characteristics

[edit]

In theTholen taxonomy, Esclangona is a common stonyS-type asteroid. It has since been characterized as a rareK-type asteroid by polarimetric observations.[19]

Rotation period

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In December 2004,photometric measurements of Esclangona made by American astronomerBrian Warner at his Palmer Divide Observatory, California, showed alightcurve with arotation period of3.247±0.002 hours and a brightness variation of0.17±0.02 inmagnitude.[13][a]

Diameter and albedo

[edit]

According to the surveys carried out by the Infrared Astronomical SatelliteIRAS, the JapaneseAkari satellite, and NASA'sWide-field Infrared Survey Explorer with its subsequentNEOWISE mission, Esclangona measures between 6.83 and 9.87 kilometers in diameter and its surface has analbedo between 0.107 and 0.41.[7][8][9][11] TheCollaborative Asteroid Lightcurve Link derives an albedo of 0.2041 and a diameter of 8.18 kilometers with anabsolute magnitude of 12.858.[4]

Naming

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Thisminor planet was named after French astronomerErnest Esclangon (1876–1954), was a director of theParis Observatory and president of theInternational Astronomical Union. Naming citation was first mentioned inThe Names of the Minor Planets byPaul Herget in 1955 (H 134).[2]

Notes

[edit]
  1. ^abLightcurve plot of 1509 Esclangona Palmer Divide Observatory,B. D. Warner (2013)
  2. ^abPravec (2009) web: Date: 2009-10-06. Rotation period3.25281±0.00002 hours with a brightness amplitude of0.13 mag. Flagged as binary. Quality code: n.a. Summary figures atCollaborative Asteroid Lightcurve Link (CALL) for (1509) Esclangona
  3. ^CALL (2011) web: rotation period5.89 hours with a brightness amplitude of0.35 mag. Quality code: n.a. Summary figures atCollaborative Asteroid Lightcurve Link (CALL) for (1509) Esclangona

References

[edit]
  1. ^abcdefgh"JPL Small-Body Database Browser: 1509 Esclangona (1938 YG)" (2016-08-27 last obs.).Jet Propulsion Laboratory. Retrieved30 June 2017.
  2. ^abcSchmadel, Lutz D. (2007). "(1509) Esclangona".Dictionary of Minor Planet Names – (1509) Esclangona.Springer Berlin Heidelberg. p. 120.doi:10.1007/978-3-540-29925-7_1510.ISBN 978-3-540-00238-3.
  3. ^abc"1509 Esclangona (1938 YG)".Minor Planet Center. Retrieved8 April 2017.
  4. ^abcdef"LCDB Data for (1509) Esclangona". Asteroid Lightcurve Database (LCDB). Retrieved8 April 2017.
  5. ^Spratt, Christopher E. (April 1990)."The Hungaria group of minor planets".Journal of the Royal Astronomical Society of Canada.84:123–131.Bibcode:1990JRASC..84..123S.ISSN 0035-872X. Retrieved8 April 2017.
  6. ^abMerline, W. J.; Close, L. M.; Dumas, C.; Chapman, C. R.; Menard, F.; Tamblyn, P. M.; et al. (May 2003)."Discovery of new asteroid binaries (121) Hermione and (1509) Esclangona".American Astronomical Society.35: 972.Bibcode:2003DPS....35.3106M. Retrieved8 April 2017.
  7. ^abcdNugent, 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. Retrieved8 April 2017.
  8. ^abcdNugent, 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.
  9. ^abcdTedesco, 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. Retrieved22 October 2019.
  10. ^abcdMarchis, F.; Enriquez, J. E.; Emery, J. P.; Mueller, M.; Baek, M.; Pollock, J.; et al. (November 2012)."Multiple asteroid systems: Dimensions and thermal properties from Spitzer Space Telescope and ground-based observations".Icarus.221 (2):1130–1161.arXiv:1604.05384.Bibcode:2012Icar..221.1130M.doi:10.1016/j.icarus.2012.09.013.hdl:2060/20130014861.S2CID 161887. Retrieved8 April 2017.
  11. ^abcdUsui, 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)
  12. ^Behrend, Raoul."Asteroids and comets rotation curves – (1509) Esclangona".Geneva Observatory. Retrieved8 April 2017.
  13. ^abWarner, Brian D. (September 2005)."Asteroid lightcurve analysis at the Palmer Divide Observatory - winter 2004-2005".The Minor Planet Bulletin.32 (3):54–58.Bibcode:2005MPBu...32...54W.ISSN 1052-8091. Retrieved8 April 2017.
  14. ^Warner, Brian D. (July 2013)."Asteroid Lightcurve Analysis at the Palmer Divide Observatory: 2013 January - March".The Minor Planet Bulletin.40 (3):137–145.Bibcode:2013MPBu...40..137W.ISSN 1052-8091.PMC 7268919.PMID 32494785. Retrieved8 April 2017.
  15. ^Polishook, D.; Brosch, N.; Prialnik, D.; Kaspi, S. (January 2009)."Simultaneous spectroscopic and photometric observations of binary asteroids".Meteoritics and Planetary Science.44 (12):1955–1966.arXiv:0909.0512.Bibcode:2009M&PS...44.1955P.doi:10.1111/j.1945-5100.2009.tb02005.x.S2CID 55167259. Retrieved8 April 2017.
  16. ^Polishook, D.; Brosch, N.; Prialnik, D. (March 2011)."Rotation periods of binary asteroids with large separations - Confronting the Escaping Ejecta Binaries model with observations".Icarus.212 (1):167–174.arXiv:1012.4810.Bibcode:2011Icar..212..167P.doi:10.1016/j.icarus.2010.12.020.S2CID 119246302. Retrieved8 April 2017.
  17. ^Warner, Brian D.; Pravec, Petr; Kusnirak, Peter; Hornoch, K.; Harris, Alan; Stephens, Robert D.; et al. (April 2010)."A Trio of Hungaria Binary Asteroids".The Minor Planet Bulletin.37 (2):70–73.Bibcode:2010MPBu...37...70W.ISSN 1052-8091. Retrieved8 April 2017.
  18. ^Gil-Hutton, R.; Lazzaro, D.; Benavidez, P. (June 2007)."Polarimetric observations of Hungaria asteroids".Astronomy and Astrophysics.468 (3):1109–1114.Bibcode:2007A&A...468.1109G.doi:10.1051/0004-6361:20077178.hdl:11336/213855.
  19. ^abBelskaya, I. N.; Fornasier, S.; Tozzi, G. P.; Gil-Hutton, R.; Cellino, A.; Antonyuk, K.; et al. (March 2017)."Refining the asteroid taxonomy by polarimetric observations".Icarus.284:30–42.Bibcode:2017Icar..284...30B.doi:10.1016/j.icarus.2016.11.003.hdl:11336/63617. Retrieved8 April 2017.
  20. ^Pravec, Petr; Harris, Alan W.; Kusnirák, Peter; Galád, Adrián; Hornoch, Kamil (September 2012)."Absolute magnitudes of asteroids and a revision of asteroid albedo estimates from WISE thermal observations".Icarus.221 (1):365–387.Bibcode:2012Icar..221..365P.doi:10.1016/j.icarus.2012.07.026. Retrieved8 April 2017.

External links

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