Main belt binary asteroidal systems with circular mutual orbits☆

Marchis, Franck; Descamps, P.; Baek, M.; Harris, Alan W.; Kaasalainen, M.; Berthier, J.; Hestroffer, Daniel; Vachier, F.

doi:10.1016/j.icarus.2008.03.007

Cited by 69 publications

(90 citation statements)

References 47 publications

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“…The binary minor planets of the LAOSA database for which we have Table 1). Two of these binary systems, (45) Eugenia (Marchis et al, 2007c) and (87) Sylvia ) are known to have additional components. To simplify this work without loss of accuracy, we did not take into consideration the tertiary component in our analyses.…”

Section: The Large Adaptive Optics Survey Of Asteroids (Laosa)mentioning

confidence: 99%

Angular momentum of binary asteroids: Implications for their possible origin

Descamps

Marchis

2008

Icarus

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We describe in this work a thorough study of the physical and orbital characteristics of extensively observed main-belt and Trojan binaries, mainly taken from the LAOSA (Large Adaptive Optics Survey of Asteroids, Marchis et al., 2006c) database, along with a selection of bifurcated objects. Dimensionless quantities, such as the specific angular momentum and the scaled primary spin rate, are computed and discussed for each system. They suggest that these asteroidal systems might be the outcome of rotational fission or mass shedding of a parent body presumably subjected to an external torque.One of the most striking features of separated binaries composed of a large primary (R p > 100 km) with a much smaller secondary (R s < 20 km) is that they all have total angular momentum of ~0.27. This value is quite close to the Maclaurin-Jacobi bifurcation (0.308) of a spinning fluid body. Alternatively, contact binaries and tidally locked double asteroids, made of components of similar size, have an angular momentum larger than 0.48. They compare successfully with the fission equilibrium sequence of a rotating fluid mass. In conclusion, we find that total angular momentum is a useful proxy to assess the internal structure of such systems.

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Section: The Large Adaptive Optics Survey Of Asteroids (Laosa)mentioning

confidence: 99%

Angular momentum of binary asteroids: Implications for their possible origin

Descamps

Marchis

2008

Icarus

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“…This gives an average density of ρ = 1.75 ± 0.30 g/cm 3 adding the 1-sigma error on the mass quadratically and propagating the 1-sigma error on the size. This density is higher than the density of multiple C-complex asteroids with a similar primary size reported in Marchis et al (2008aMarchis et al ( , 2008b …”

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confidence: 50%

Characteristics and large bulk density of the C-type main-belt triple asteroid (93) Minerva

Marchis¹,

Vachier²,

Ďurech³

et al. 2013

Icarus

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Abstract:From a set of adaptive optics (AO) observations collected with the W.M. Keck telescope between August and September 2009, we derived the orbital parameters of the most recently discovered satellites of the large C-type asteroid (93) Minerva. The satellites of Minerva, which are approximately 3 and 4 km in diameter, orbit very close to the primary (~5 & ~8 × R p and ~1% & ~2% × R Hill ) in a circular manner, sharing common characteristics with most of the triple asteroid systems in the main-belt. Combining these AO observations with lightcurve data collected since 1980 and two stellar occultations in 2010 & 2011, we removed the ambiguity of the pole solution of Minerva's primary and showed that it has an almost regular shape with an equivalent diameter D eq = 154 ± 6 km in agreement with IRAS observations. The surprisingly high bulk density of 1.75 ± 0.30 g/cm 3 for this C-type asteroid, suggests that this taxonomic class is composed of asteroids with different compositions, For instance, Minerva could be made of the same material as dry CR, CO, and CV meteorites. We discuss possible scenarios on the origin of the system and conclude that future observations may shine light on the nature and composition of this fifth known triple main-belt asteroid. Keyword:Asteroids -Satellites of asteroids -Adaptive optics -Photometry -Orbit determination -Interior 1 Introduction The serendipitous discovery of Dactyl, a companion of the main-belt asteroid (243) Ida, seen during the Galileo spacecraft voyage to Jupiter (Chapman et al. 1995), gave birth to a new field of study for small solar system bodies. Today, using techniques such as high angular resolution imaging with the Hubble Space Telescope (HST), adaptive optics (AO) on ground-based telescopes, radar observations and photometric studies, about 200 multiple asteroids (asteroids with one or several moons) are known in all populations of small solar system bodies, from the Near-Earth Asteroids to the Kuiper Belt Objects. The study of these multiple asteroids is an opportunity for planetary astronomers to obtain insights on the asteroids such as their masses and densities and how these quantities possibly relate to their compositions, see e.g. Marchis et al. 2012a. Their existence and the understanding of their formation and evolution also provide a direct window to the history of our solar system. In this work, we describe a study of one of these recently discovered triple asteroid systems. (93) Minerva is a large (H v = 7.7, P spin = 5.97909 hours in Tungalag 2002) asteroid discovered by J.C. Watson at Ann Arbor, MI, USA in 1867. Located in the middle of the main-belt (a Minerva = 2.75 AU, e Minerva = 0.14, i Minerva = 9 deg), it was initially classified as a member of an old collisional family (1.2 ± 0.4 Gyrs) named "Gefion" consisting of 973 members based on Nesvorny et al. (2005). Because most of the members of this family are identified as S-type, and (93) Minerva is known to be a C b -type (Lazarro et al. 2004) Ryan & Woodward, 2010). There is a clear ...

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“…The cleaned map reflects the signal strength expected for a rotation-limited integration time of 5 min. Kleopatra's two satellites (Marchis et al, 2008) are outside the bounds of this image, and both have fluxes only slightly above the noise. simulation are shown in Fig.…”

Section: Alma Snapshot Imaging Of Asteroidsmentioning

confidence: 95%

“…Therefore, I have simulated an ALMA 750 GHz (0.4 mm) continuum image of the main-belt asteroid 216 Kleopatra, whose shape has been modeled from radar observations (Ostro et al, 2000) validated by adaptive optics images (Marchis et al, 2008). My simulation includes only Kleopatra itself, and not Color contours are relative flux or scaled brightness temperature computed assuming zero thermal inertia and a Lambertian surface, for illustration purposes only.…”

Section: Alma Snapshot Imaging Of Asteroidsmentioning

confidence: 99%

ALMA and asteroid science

Busch

2009

Icarus

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Main belt binary asteroidal systems with circular mutual orbits☆

Cited by 69 publications

References 47 publications

Angular momentum of binary asteroids: Implications for their possible origin

Angular momentum of binary asteroids: Implications for their possible origin

Characteristics and large bulk density of the C-type main-belt triple asteroid (93) Minerva

ALMA and asteroid science

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