90 Antiope

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90 Antiope
90 Antiope.gif
Adaptive-optics image of Antiope
Discovery [1]
Discovered byRobert Luther
Discovery dateOctober 1, 1866
1952 BK2[1]
Main belt[1]
(Themis family)
Orbital characteristics[1]
Epoch July 23, 2010
(JD 2455400.5)
Aphelion545.94 Gm
3.6494 AU
Perihelion398.02 Gm
2.6606 AU
471.19 Gm
3.1550 AU
2046.9 d (5.60 yr)
16.66 km/s
Physical characteristics
Dimensions93.0×87.0×83.6 km[2]
87.8 ± 1.0 km[2]
Mass8.3×1017 kg
(whole system)[3]
~ 4.1−4.2 ×1017 kg (components)
Mean density
1.25 ± 0.05 g/cm³ (each)[4]
Equatorial surface gravity
variable; ~ 0.03−0.04 m/s²
Equatorial escape velocity
variable; ~ 35−40 m/s
0.687 d (16.50 h)[5] (synchronous)
Surface temp. min mean max
Kelvin ~158 K 244 K
Celsius -115 C -29°
8.27 (together)[1]
9.02 (each component)

90 Antiope (/[invalid input: 'icon']ænˈt.əp/ an-TY-ə-pee) is a double asteroid in the outer asteroid belt. It was discovered on October 1, 1866, by Robert Luther. In 2000 it was found to consist of two almost-equally-sized bodies orbiting each other. At average diameters of about 88 km and 84 km, both components are among the 500 largest asteroids. Antiope is a member of the Themis family of asteroids that share similar orbital elements.[8]


The number in 90 Antiope's name denotes that it was the 90th asteroid to be discovered. Its proper name comes from Greek mythology, though it is disputed as to whether this is Antiope the Amazon or Antiope the mother of Amphion and Zethus.

Since the discovery of Antiope's binary nature, the name "Antiope" technically refers to the slightly larger of the two components, with the smaller component bearing the provisional designation S/2000 (90) 1. However, the name "Antiope" is also used to refer to the binary system as a whole.


The most remarkable feature of Antiope is that it consists of two components of almost equal size (the difference in mass is less than 2.5%[9]), making it a truly "double" asteroid. Its binary nature was discovered on 10 August 2000 by a group of astronomers using adaptive optics at the Keck Telescope on Mauna Kea.[10] Before this, IRAS observations had suggested that the asteroid was 120 km in diameter.[1]


Antiope orbits in the outer third of the core region of the asteroid belt, and is a member of the Themis family.

Since each component is about 86±1 km across, with their centers separated by only about 171 kilometers,[3] the gap separating the two halves is about the same as the diameter of each component. As a result, the two bodies orbit around the common center of mass which lies in the space between them. The orbital period is approximately 16.50 hours, and the eccentricity below 0.006.[3] Every several years, a period of mutual occultations occurs when the asteroid is viewed from Earth.[5] Using Kepler's third law, the mass and density of the components can be derived from the orbital period and component sizes.

The axis of the mutual orbit of the two components points towards ecliptic coordinates (β, λ) = (200°, 38°)[4] with 2 degrees uncertainty.[4] This is tilted about 63° to the circumsolar orbit of the system.


Antiope itself has an average diameter of about 88 km, while its twin, S/2000 90 (1), has an average diameter of 84 km. Like most bodies in this region, the components of the Antiope system are of the dark C spectral type, indicating a carbonaceous composition. The low density (1.3±0.2 g/cm³) of its components (see below) suggests a significant porosity (>30%), indicating rubble-pile asteroids composed of debris that accumulated in the aftermath of a previous asteroid collision, possibly the one that formed the Themis family.[citation needed]

Complementary observations using adaptive optic observations on 8–10m class telescopes and mutual events photometric lightcurve over several months have served as input quantities for a derivation of a whole set of other physical parameters (shapes of the components, surface scattering, bulk density, and internal properties). The shape model is consistent with slightly non-spherical components, having a size ratio of 0.95 (with an average radius of 42.9 km), and exhibiting equilibrium figures for homogeneous rotating bodies. A comparison with grazing occultation event lightcurves taken in 2003 suggests that the real shape of the components do not depart much from Roche equilibrium figures (by more than 10%).[citation needed]

Observations from the VLT-UT4 telescope equipped with an adaptive optics system in 2007 and lightcurve data analysis suggest that one of the components appears to have a 68-km bowl-shaped impact crater that may be the result of a violent collision of proto-Antiope into two equisized bodies.[11] The impactor is calculated to have been more than 17 km in diameter.[12] The crater can not be resolved using the W.M. Keck II telescope, but has been confirmed by the occultation of the star LQ Aquarii on 2011 July 19 10:25UT.[13]

One observed stellar occultation by Antiope was reported, on June 11, 1980. On 2011 July 19 10:25UT, Antiope was observed to occult a magnitude 6.7 star for up to about 30 seconds.[14]

S/2000 (90) 1
Discovered byW. J. Merline, L. M. Close,
J. C. Shelton, C. Dumas,
F. Menard, C. R. Chapman,
and D. C. Slater
Discovery dateAugust 10, 2000[15]
Main belt (Themis family)
Orbital characteristics[3]
171 ± 1 km
0.687713 ± 0.00004 d (16.5051 ± 0.0001 h)
18.0 m/s
Satellite ofBinary with 90 Antiope
Physical characteristics
Dimensions89.4×82.8×79.6 km[2]
83.8 ± 1.0 km[2]
Mass~ 8.1−8.5 ×1017 kg[4]
Equatorial escape velocity
variable; ~ 35−40 m/s
0.687 d (16.50 h)[5] (synchronous)


  1. ^ a b c d e "JPL Small-Body Database Browser: 90 Antiope". 2010-06-13 last obs. Retrieved 2010-07-08. Check date values in: |date= (help)
  2. ^ a b c d Wm. Robert Johnston (2008-11-23). "(90) Antiope and S/2000 (90) 1". Johnston's Archive. Retrieved 2008-01-23.
  3. ^ a b c d 90 Antiope A & B, online data sheet, F. Marchis
  4. ^ a b c d Descamps et al., 2007, Icarus article published in April 2007
  5. ^ a b c "T. Michałowski; et al. (2004). "Eclipsing binary asteroid 90 Antiope". Astronomy & Astrophysics. 423 (3): 1159. Bibcode:2004A&A...423.1159M. doi:10.1051/0004-6361:20040449. Unknown parameter |author-separator= ignored (help)
  6. ^ Supplemental IRAS Minor Planet Survey
  7. ^ PDS spectral class data
  8. ^ Moore, Patrick; Rees, Robin, eds. (2011), Patrick Moore's Data Book of Astronomy (2nd ed.), Cambridge University Press, p. 165.
  9. ^ F. Marchis, F. Descamps, P. Hestroffer, and I. de Pater; Descamps; Hestroffer; Berthier; De Pater (2004). "Fine Analysis of 121 Hermione, 45 Eugenia, and 90 Antiope Binary Asteroid Systems With AO Observations". Bulletin of the American Astronomical Society. 36: 1180. Bibcode:2004DPS....36.4602M.CS1 maint: Multiple names: authors list (link)
  10. ^ a b IAUC 7503
  11. ^ Marchis, Franck (2009). The Origin of the Double Main Belt Asteroid (90) Antiope by Component-Resolved Spectroscopy. DPS meeting #41. American Astronomical Society. Retrieved 2009-11-08. Unknown parameter |coauthors= ignored (|author= suggested) (help)
  12. ^ Descamps, P. (2009). "A giant crater on 90 Antiope?". Icarus. 203 (1): 102–111. arXiv:0905.0631. Bibcode:2009Icar..203..102D. doi:10.1016/j.icarus.2009.04.022. Unknown parameter |coauthors= ignored (|author= suggested) (help)
  13. ^ Antiope Occultation Yields Double Bonanza. Sky & Telescope
  14. ^ Franck Marchis (July 21, 2011). "An Occultation by the double asteroid (90) Antiope seen in California". NASA blog (Cosmic Diary). Retrieved 2012-01-28.
  15. ^ "90 Antiope: Raw Keck Image". SWrI Press Release. August 2000. Retrieved 2009-10-20.

External links