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1509 Esclangona

1509 Esclangona, provisional designation 1938 YG, is a rare-type Hungaria asteroid and binary system from the inner regions of the asteroid belt, approximately 8 kilometers in diameter. It is named after French astronomer Ernest Esclangon.

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)
Aphelion1.9263 AU
Perihelion1.8064 AU
1.8663 AU
Eccentricity0.0321
2.55 yr (931 days)
225.08°
0° 23m 11.76s / day
Inclination22.320°
283.52°
267.82°
Known satellites1[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]
5.89 h[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]

Discoveries

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Esclangona was discovered on 21 December 1938, by French astronomer André Patry at Nice Observatory. The body's observation arc begins with its official discovery observation as no precoveries were taken, and no prior identifications were made.[3] On 13 February 2003, a minor-planet moon in orbit of Esclangona was discovered by astronomers at ESO's Very Large Telescope (UT4) on Cerro Paranal in Chile.[2][3]

Orbit and classification

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Esclangona is a member of the Hungaria family, which form the innermost concentration of asteroids in the Solar System. It orbits the Sun in the inner main-belt at a distance of 1.8–1.9 AU once every 2 years and 7 months (931 days). Its orbit has an eccentricity of 0.03 and an inclination of 22° with respect to the ecliptic.[1]

Binary system

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Esclangona has a small moon, provisionally named S/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 are ejecta from an asteroidal collision in the past that left the scene as a co-orbiting pair; a similar pairing is 3749 Balam and its moon.[6]

Physical characteristics

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In the Tholen taxonomy, Esclangona is a common stony S-type asteroid. It has since been characterized as a rare K-type asteroid by polarimetric observations.[19]

Rotation period

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In December 2004, photometric measurements of Esclangona made by American astronomer Brian Warner at his Palmer Divide Observatory, California, showed a lightcurve with a rotation period of 3.247±0.002 hours and a brightness variation of 0.17±0.02 in magnitude.[13][a]

Diameter and albedo

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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, Esclangona measures between 6.83 and 9.87 kilometers in diameter and its surface has an albedo between 0.107 and 0.41.[7][8][9][11] The Collaborative Asteroid Lightcurve Link derives an albedo of 0.2041 and a diameter of 8.18 kilometers with an absolute magnitude of 12.858.[4]

Naming

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This minor planet was named after French astronomer Ernest Esclangon (1876–1954), was a director of the Paris Observatory and president of the International Astronomical Union. Naming citation was first mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 134).[2]

Notes

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  1. ^ a b Lightcurve plot of 1509 Esclangona Palmer Divide Observatory, B. D. Warner (2013)
  2. ^ a b Pravec (2009) web: Date: 2009-10-06. Rotation period 3.25281±0.00002 hours with a brightness amplitude of 0.13 mag. Flagged as binary. Quality code: n.a. Summary figures at Collaborative Asteroid Lightcurve Link (CALL) for (1509) Esclangona
  3. ^ CALL (2011) web: rotation period 5.89 hours with a brightness amplitude of 0.35 mag. Quality code: n.a. Summary figures at Collaborative Asteroid Lightcurve Link (CALL) for (1509) Esclangona

References

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  1. ^ a b c d e f g h "JPL Small-Body Database Browser: 1509 Esclangona (1938 YG)" (2016-08-27 last obs.). Jet Propulsion Laboratory. Retrieved 30 June 2017.
  2. ^ a b c Schmadel, 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. ^ a b c "1509 Esclangona (1938 YG)". Minor Planet Center. Retrieved 8 April 2017.
  4. ^ a b c d e f "LCDB Data for (1509) Esclangona". Asteroid Lightcurve Database (LCDB). Retrieved 8 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. Retrieved 8 April 2017.
  6. ^ a b Merline, 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. Retrieved 8 April 2017.
  7. ^ a b c d 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 April 2017.
  8. ^ a b c d 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.
  9. ^ a b c d 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.
  10. ^ a b c d Marchis, 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. Retrieved 8 April 2017.
  11. ^ a b c d 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)
  12. ^ Behrend, Raoul. "Asteroids and comets rotation curves – (1509) Esclangona". Geneva Observatory. Retrieved 8 April 2017.
  13. ^ a b Warner, 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. Retrieved 8 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. Retrieved 8 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. Retrieved 8 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. Retrieved 8 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. Retrieved 8 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. ^ a b Belskaya, 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. Retrieved 8 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. Retrieved 8 April 2017.
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