Component-resolved near-infrared spectra of the (22) Kalliope system

Laver, Conor; Pater, Imke de; Marchis, Franck; Ádámkovics, Máté; Wong, Michael H.

doi:10.1016/j.icarus.2009.07.002

Cited by 16 publications

(13 citation statements)

References 17 publications

(36 reference statements)

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“…Such a scenario was already proposed to explain the binary nature of the Asteroid 22 Kalliope and was recently substantiated by new spectroscopic observations of both components revealing the same surface composition (Laver et al, 2009). From Weidenschilling et al (1989) we have computed the tidal evolution time scales as a function of the relative separation, and mass ratio.…”

Section: Discussionmentioning

confidence: 63%

Triplicity and physical characteristics of Asteroid (216) Kleopatra

Descamps

Marchis

Berthier

et al. 2011

Icarus

101

121

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a b s t r a c tTo take full advantage of the September 2008 opposition passage of the M-type Asteroid (216) Kleopatra, we have used near-infrared adaptive optics (AO) imaging with the W.M. Keck II telescope to capture unprecedented high resolution images of this unusual asteroid. Our AO observations with the W.M. Keck II telescope, combined with Spitzer/IRS spectroscopic observations and past stellar occultations, confirm the value of its IRAS radiometric radius of 67.5 km as well as its dog-bone shape suggested by earlier radar observations. Our Keck AO observations revealed the presence of two small satellites in orbit about Kleopatra (see Marchis, F. et al. Circ. 8980). Accurate measurements of the satellite orbits over a full month enabled us to determine the total mass of the system to be 4.64 ± 0.02 Â 10 18 kg. This translates into a bulk density of 3.6 ± 0.4 g/cm 3 , which implies a macroscopic porosity for Kleopatra of $30-50%, typical of a rubble-pile asteroid. From these physical characteristics we measured its specific angular momentum, very close to that of a spinning equilibrium dumbbell.

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Section: Discussionmentioning

confidence: 63%

Triplicity and physical characteristics of Asteroid (216) Kleopatra

Descamps

Marchis

Berthier

et al. 2011

Icarus

101

121

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“…Spectra of (22) Kalliope and its satellite Linus in the 1-2.4 µm region appear to be similar (Laver et al 2009), which the authors attribute to satellite formation after a major impact on the precursor body. Observations of both components of (90) Antiope in the same spectral region also shows surface reflectances that are similar .…”

Section: Spectral Observations Of Mba and Trojan Systemsmentioning

confidence: 83%

Asteroid Systems: Binaries, Triples, and Pairs

et al. 2015

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In the past decade, the number of known binary near-Earth asteroids has more than quadrupled and the number of known large main belt asteroids with satellites has doubled. Half a dozen triple asteroids have been discovered, and the previously unrecognized populations of asteroid pairs and small main belt binaries have been identified. The current observational evidence confirms that small (<20 km) binaries form by rotational fission and establishes that the YORP effect powers the spin-up process. A unifying paradigm based on rotational fission and post-fission dynamics can explain the formation of small binaries, triples, and pairs. Large (>20 km) binaries with small satellites are most likely created during large collisions.Comment: 31 pages, 12 figures. Chapter in the book ASTEROIDS IV (in press

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“…We are confident, however, that the satellite is not of a significantly different taxonomic type. We have presented the third resolved spectrum of a moonlet satellite of a multiple asteroid system, the first being (22) Kalliope from Laver et al (2009) and the second, (90) Antiope ). Our innovative extraction method allows us to derive the spectra of the satellite (with a magnitude difference of 5 and distance of 1.5 ′′ ) and the primary, and this method could be used for similar future projects.…”

Section: Resultsmentioning

confidence: 99%

A spectral comparison of (379) Huenna and its satellite

DeMeo¹,

Carry²,

Marchis³

et al. 2011

Icarus

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We present near-infrared spectral measurements of Themis family asteroid (379) Huenna (D~98 km) and its 6 km satellite using SpeX on the NASA IRTF. The companion was farther than 1.5" from the primary at the time of observations and was approximately 5 magnitudes dimmer. We describe a method for separating and extracting the signal of a companion asteroid when the signal is not entirely resolved from the primary. The spectrum of (379) Huenna has a broad, shallow feature near 1 {\mu}m and a low slope, characteristic of C-type asteroids. The secondary's spectrum is consistent with the taxonomic classification of C-complex or X-complex. The quality of the data was not sufficient to identify any subtle feature in the secondary's spectrum.Comment: 6 pages, 4 figures, 2 tables - Accepted for publication in Icaru

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Component-resolved near-infrared spectra of the (22) Kalliope system

Cited by 16 publications

References 17 publications

Triplicity and physical characteristics of Asteroid (216) Kleopatra

Triplicity and physical characteristics of Asteroid (216) Kleopatra

Asteroid Systems: Binaries, Triples, and Pairs

A spectral comparison of (379) Huenna and its satellite

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