Main-belt asteroid (M-type) · Central main belt · ≈ 2.8 AU

Kleopatra

(216) Kleopatra · discovered 1880 at Pola

A 270-kilometre “dog bone” with two little moons named after Cleopatra’s twins.

Kleopatra at a glance
Object typeMain-belt asteroid, Tholen M-type / SMASS Xe[1]
DiscoveredApril 10, 1880 by Johann Palisa at Pola (now Pula, Croatia)[2]
Named forCleopatra VII of Egypt[2]
Dimensions≈ 276 × 94 × 78 km[1]
Mean diameter≈ 120–122 km (volume-equivalent)[2]
Mass(2.97 ± 0.32) × 10¹⁸ kg[2]
Density3.38 ± 0.50 g/cm³[2]
Rotation period≈ 5.39 hours[1]
MoonsAlexhelios (≈ 8.9 km, 2.7 d) and Cleoselene (≈ 6.9 km, 1.8 d)[2]
Distance from Sun2.10–3.49 AU[1]
Orbital period≈ 4.7 years[1]
Inclination≈ 13.1°[1]

The dog-bone asteroid

Kleopatra is one of the strangest-looking objects in the asteroid belt: about 276 km long but under 100 km wide, with two lobes joined by a thinner middle.[1] Its volume-equivalent diameter is only about 120 km.[2]

The elongation first showed up in a 1991 stellar occultation timed from eight locations. Later radar observations at Arecibo showed the two lobes are connected, like a ham-bone, and the resulting shape model made the cover of Science.[2][5]

Alexhelios and Cleoselene

A 1988 search for moons came up empty. Then in September 2008, Franck Marchis and colleagues announced two moons found with the Keck Observatory’s adaptive optics.[2]

In 2011 they were named after Cleopatra’s twin children: Alexhelios (outer, about 8.9 km, 2.7-day orbit) and Cleoselene (inner, about 6.9 km, 1.8-day orbit).[2]

Metal — but how much?

Kleopatra is an M-type asteroid, a class often linked to metal.[4] Its moons allow its mass to be measured: (2.97 ± 0.32) × 1018 kg, lower than earlier thought, and a bulk density of 3.38 ± 0.50 g/cm³.[2]

That density questions the old picture of a pure metal body. Radar suggests metal-rich material in the south but more ordinary rock along the equator. One explanation is a porous rubble pile with a lot of metal mixed in.[2][6]

Spun into shape

One idea explains shape, spin and moons at once: an oblique impact, perhaps 100 million years ago, spun Kleopatra up, stretched it out and flung off Alexhelios; Cleoselene may have split off around 10 million years ago.[2]

Kleopatra is a contact binary — if it spun much faster, the two lobes would separate and become a true binary system.[2][7]

Meteorite buying guide

Metal-rich asteroids like Kleopatra are related to the iron meteorites you can actually hold. Answer five quick questions and we’ll suggest specimen types that match your budget and interests — with links to browse current listings.

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Orbit

Kleopatra belongs to the background population of the central belt rather than any family. It orbits between about 2.1 and 3.5 AU every 4.7 years, tilted 13°.[2][1]

Sun Earth (1 AU)Mars (1.52 AU) aphelion ≈ 3.49 AU perihelion ≈ 2.10 AU
Top-down orbit of Kleopatra to scale, computed from JPL orbital elements (a ≈ 2.8 AU, e ≈ 0.25).[1] Earth and Mars orbits shown for comparison.[10]

Holding a piece of an asteroid

No meteorite is known to come from Kleopatra, but iron and stony-iron meteorites do come from metal-rich asteroids. Our meteorite buying guide explains the main types and how to buy a genuine specimen.[4]

Read more

Sources

  1. Small-Body Database Lookup: 216 Kleopatra — NASA JPL Solar System Dynamics
  2. 216 Kleopatra — Wikipedia
  3. Johann Palisa — Wikipedia
  4. M-type asteroid — Wikipedia
  5. Arecibo Telescope — Wikipedia
  6. Rubble pile — Wikipedia
  7. Contact binary (small Solar System body) — Wikipedia
  8. Occultation — Wikipedia
  9. Small-Body Database Lookup: 16 Psyche — NASA JPL Solar System Dynamics
  10. Planetary Fact Sheet (orbit comparison) — NASA NSSDCA

Figures are rounded; where sources differ we note it. Spotted an error? Tell us.