96 Aegle

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96 Aegle
Discovery [1]
Discovered byJ. Coggia
Discovery siteMarseille Obs.
Discovery date17 February 1868
MPC designation(96) Aegle
Pronunciation/ˈɡli/ · EE-glee
Named after
Aegina (Greek mythology)[2][a]
main-belt[1][3] · (outer)[4]
Orbital characteristics[3]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc149.92 yr (54,760 d)
Aphelion3.4796 AU
Perihelion2.6251 AU
3.0524 AU
5.33 yr (1,948 d)
0° 11m 5.28s / day
Physical characteristics
Dimensions178.7 km × 148.3 km[b]
Mean diameter
156 km[6]
162.85 km (calculated)[4]
164.77±2.54 km[7]
167.92±5.49 km[8]
170.02±3.4 km[9]
177.77±1.54 km[10]
Mass(6.48±6.26)×1018 kg[8]
Mean density
2.61±2.53 g/cm3[8]
10 h (poor)[11]
10.470 h (poor)[12]
13.82±0.01 h[13]
13.82±0.01 h[14]
13.868±0.001 h[15][c]
26.53±0.01 h (poor)[16]
0.058 (assumed)[4]
Tholen = T[3]
SMASS = T[3][4]
Bus–DeMeo = T[17]
B–V = 0.775[3]
U–B = 0.337[3]
7.54[16] · 7.65[4]

Aegle (/ˈɡli/ EE-glee; minor planet designation: 96 Aegle) is a carbonaceous asteroid and the namesake of the Aegle family located in the outer regions of the asteroid belt, approximately 170 kilometers (110 miles) in diameter. It was discovered on 17 February 1868, by French astronomer Jérôme Coggia at the Marseille Observatory in southeastern France.[1] The rare T-type asteroid has a rotation period of 13.8 hours and has been observed several times during occultation events.[4] It was named after the river nymph Aegina (Aigle, Aegle) from Greek mythology.[2][a]

Orbit and classification[edit]

Aegle is the parent body of the Aegle family (630), a very small asteroid family of less than a hundred known members.[5][19]:23 It orbits the Sun in the outer asteroid belt at a distance of 2.6–3.5 AU once every 5 years and 4 months (1,948 days; semi-major axis of 3.05 AU). Its orbit has an eccentricity of 0.14 and an inclination of 16° with respect to the ecliptic.[3] The body's observation arc begins at Litchfield Observatory (789) in August 1870, two and a half years after its official discovery observation at Marseille.[1]

Physical characteristics[edit]

In both the Tholen and SMASS classification as well as in the Bus–DeMeo taxonomy, Aegle is a rare, anhydrous T-type asteroid,[3] while the overall spectral type for the Aegle family is typically that of a C- and X-type.[19]:23

Rotation period[edit]

Photometric observations of the asteroid by American photometrist Frederick Pilcher from his Organ Mesa Observatory (G50) in New Mexico during 2016−17 showed an irregular lightcurve with a synodic rotation period of 13.868 hours and an amplitude of 0.11 in magnitude (U=3).[15][c]

This result is in good agreement with two previous observations by Robert Stephens, and by Cyril Cavadore and Pierre Antonini who measured a period of 13.82 hours and a brightness variation of 0.12 and 0.05, respectively (U=3/2-).[14][13] Other rotational lightcurves obtained by Alan Harris (10 h; 1980),[11] by Italian (10.47 h; 2000),[12] and Swiss/French astronomers (13.82 h; 2005),[14] and at the Colgate University (26.53 h; 2001),[16] are of poor quality (U=n.a./1/1/1).[4]

Diameter and albedo[edit]

According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Aegle measures between 156 and 178 kilometers in diameter and its surface has a low albedo between 0.048 and 0.056.[6][7][9][10] The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.058 and calculates a diameter of 162.85 kilometers based on an absolute magnitude of 7.65.[4] It has an estimated mass of (6.48±6.26)×1018 kg with a density of 2.61±2.53 g/cm3.[8]


Aegle has been observed occulting stars several times. On 5 January 2010, it occulted the star TYC 0572-01644-1 as seen from Ibaraki, Japan, and allowed to determine a cross-section of 178.7 × 148.3 kilometers.[b] In New Zealand, on 18 February 2002, it occulted the star TYC 7299-00684 in the constellation of Centaurus for approximately 12.7 seconds during which a drop of 2.1 in magnitude was to be expected.[d]


This minor planet was named after the river nymph Aegina (/iˈnə/, also known as Aigle or Aegle) one of the three Hesperidess in Greek mythology. Aegina is the daughter of the river-god Asopus and the nymph Metope. She was changed into the Greek island of Aegina by Zeus, who fathered her son King Aeacus. The official naming citation was mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 13).[2][a]


  1. ^ a b c The Dictionary of Minor Planet Names cited in a previous edition: "Named after the daughter of Asopus, a son of Poseidon. She was changed by Zeus, father of one of her sons, into the island bearing her name (H13). Named by C. Bruhns, 1868, published in the Astronomische Nachrichten AN 37, 71.
  2. ^ a b Occultation by (96) Aegle on 5 January 2010. Occulted star: TYC 0572-01644-1. Derived asteroid dimension: 178.7 km × 148.3 km. Successful observations on the Sendai Space Hall.
  3. ^ a b Lightcurve plot of (96) Aegle, by Frederick Pilcher (2017) at the Organ Mesa Observatory (G50), with rotation period 13.868±0.001 hours. Quality code of 3. Summary figures at the LCDB and at Pilcher's ASLC project page.
  4. ^ Occultation by (96) Aegle on 18 February 2002. Occulted star: TYC 7299-00684. Max duration 12.7 sec. Δmag 2.1. Diameter est. 168 km. Sourced from the Occultation Section of the Royal Astronomical Society of New Zealand (path prediction).


  1. ^ a b c d "96 Aegle". Minor Planet Center. Retrieved 28 March 2018.
  2. ^ a b c Schmadel, Lutz D. (2007). Dictionary of Minor Planet Names – (96) Aegle. Springer Berlin Heidelberg. p. 24. ISBN 978-3-540-00238-3. Retrieved 28 March 2018.
  3. ^ a b c d e f g h i "JPL Small-Body Database Browser: 96 Aegle" (2018-01-24 last obs.). Jet Propulsion Laboratory. Retrieved 28 March 2018.
  4. ^ a b c d e f g h "LCDB Data for (96) Aegle". Asteroid Lightcurve Database (LCDB). Retrieved 28 March 2018.
  5. ^ a b "Small Bodies Data Ferret". Nesvorny HCM Asteroid Families V3.0. Retrieved 28 March 2018.
  6. ^ a b Marchis, F.; Kaasalainen, M.; Hom, E. F. Y.; Berthier, J.; Enriquez, J.; Hestroffer, D.; et al. (November 2006). "Shape, size and multiplicity of main-belt asteroids. I. Keck Adaptive Optics survey". Icarus. 185 (1): 39–63. Bibcode:2006Icar..185...39M. doi:10.1016/j.icarus.2006.06.001. PMC 2600456. Retrieved 28 March 2018.
  7. ^ 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. Retrieved 28 March 2018. Online catalog
  8. ^ a b c d Carry, B. (December 2012), "Density of asteroids" (PDF), Planetary and Space Science, 73, pp. 98–118, arXiv:1203.4336, Bibcode:2012P&SS...73...98C, doi:10.1016/j.pss.2012.03.009 See Table 1.
  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. Bibcode:2004PDSS...12.....T. Archived from the original on 3 June 2016. Retrieved 28 March 2018.
  10. ^ a b c d Masiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Nugent, C.; et al. (November 2012). "Preliminary Analysis of WISE/NEOWISE 3-Band Cryogenic and Post-cryogenic Observations of Main Belt Asteroids". The Astrophysical Journal Letters. 759 (1): 5. arXiv:1209.5794. Bibcode:2012ApJ...759L...8M. doi:10.1088/2041-8205/759/1/L8. Retrieved 28 March 2018.
  11. ^ a b c Harris, A. W.; Young, J. W. (October 1989). "Asteroid lightcurve observations from 1979-1981". Icarus: 314–364. Bibcode:1989Icar...81..314H. doi:10.1016/0019-1035(89)90056-0. ISSN 0019-1035. Retrieved 28 March 2018.
  12. ^ a b Blanco, C.; Di Martino, M.; Riccioli, D. (April 2000). "New rotational periods of 18 asteroids". Planetary and Space Science. 48 (4): 271–284. Bibcode:2000P&SS...48..271B. doi:10.1016/S0032-0633(99)00074-4. Retrieved 28 March 2018.
  13. ^ a b Stephens, Robert D. (March 2005). "Rotational periods of 96 Aegle, 386 Siegena, 390 Alma, 544 Jetta, 2771 Polzunov, and (5917) 1991 NG". The Minor Planet Bulletin. 32 (1): 2–3. Bibcode:2005MPBu...32....2S. ISSN 1052-8091. Retrieved 28 March 2018.
  14. ^ a b c Behrend, Raoul. "Asteroids and comets rotation curves – (96) Aegle". Geneva Observatory. Retrieved 28 March 2018.
  15. ^ a b Pilcher, Frederick (July 2017). "Rotation Period Determinations for 49 Pales, 96 Aegle, 106 Dione 375 Ursula, and 576 Emanuela". The Minor Planet Bulletin. 44 (3): 249–251. Bibcode:2017MPBu...44..249P. ISSN 1052-8091. Retrieved 28 March 2018.
  16. ^ a b c Slivan, S. M.; Roller, E. A. (December 2001). "New Lightcurve Observations of 96 Aegle". The Minor Planet Bulletin. 28: 69–71. Bibcode:2001MPBu...28...69S. Retrieved 28 March 2018.
  17. ^ DeMeo, Francesca E.; Binzel, Richard P.; Slivan, Stephen M.; Bus, Schelte J. (July 2009). "An extension of the Bus asteroid taxonomy into the near-infrared" (PDF). Icarus. 202 (1): 160–180. Bibcode:2009Icar..202..160D. doi:10.1016/j.icarus.2009.02.005. Archived from the original (PDF) on 17 March 2014. Retrieved 23 June 2017. (Catalog Archived 29 March 2018 at the Wayback Machine. at PDS)
  18. ^ 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 28 March 2018.
  19. ^ a b Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families" (PDF). Asteroids IV: 297–321. arXiv:1502.01628. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. Retrieved 28 March 2018.

External links[edit]