Mass and density of Asteroid 121 Hermione from an analysis of its companion orbit

Marchis, Franck; Hestroffer, Daniel; Descamps, P.; Berthier, J.; Laver, Conor; Pater, I. de

doi:10.1016/j.icarus.2005.05.003

Cited by 38 publications

(33 citation statements)

References 27 publications

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“…The bi-lobed structure of 121 Hermione observed by Marchis et al (2005c) was confirmed in this study. The proportion of contact binaries in our survey which is limited to asteroids larger than 40 km is surprisingly high (∼6%).…”

Section: Resultssupporting

confidence: 85%

“…This shape is quite similar to the one proposed for 121 Hermione, another bi-lobed main-belt asteroid that was also observed with the Keck AO telescope (Marchis et al, 2005c). Bifurcated shapes in the near-Earth asteroid population are quite common and have been seen through radar observations [see review in Ostro et al (2002)].…”

Section: Klymenesupporting

confidence: 79%

“…An accurate determination of the orbital parameters of such system require a long term program of observations spanning several years. This task was initiated a few years ago by our group; and we have thus far measured the orbits of 22 Kalliope and Linus (Marchis et al, 2003a), 45 Eugenia and Petit-Prince (Marchis et al, 2004b), 87 Sylvia and its two moonlets (Marchis et al, 2005b) and 121 Hermione and "LaFayette" [proposed name for S/ 2002 (121) 1] (Marchis et al, 2005c). Additional estimated orbits for the companions of 107 Camilla, 379 Huenna, and 3749 Balam have been proposed by Marchis et al (2005a).…”

Section: Search For Moonlet Companionsmentioning

confidence: 99%

“…121 Hermione- Marchis et al (2005c) present a detailed analysis of this asteroid system considering additional observations recorded with the VLT AO system, including the orbital elements of its secondary, the shape of the primary and a comparison with an ellipsoid shape model. The analysis reported here using a different deconvolution method confirms the bilobated shape of the asteroid and its apparent size.…”

Section: Other Asteroidsmentioning

confidence: 99%

“…The design and performance of AO systems have continued to mature, so as to provide more stable correction on fainter targets. It is now possible by ground-based AO instrumentation to resolve several main-belt asteroids which are very close to the diffraction limit of an 8-10 m telescope (typically ∼60 mas, corresponding to main-belt asteroids with D > 50 km), enabling us to study the size and shape of small asteroids (e.g., Conrad et al, 2003;Marchis et al, 2004bMarchis et al, , 2005aMarchis et al, , 2005bMarchis et al, , 2005c and to map the surface of larger asteroids (e.g., 4 Vesta; Zellner et al, 2005).…”

Section: Introductionmentioning

confidence: 99%

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Shape, size and multiplicity of main-belt asteroidsI. Keck Adaptive Optics survey

Marchis

Kaasalainen

Hom

et al. 2006

Icarus

109

101

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This paper presents results from a high spatial resolution survey of 33 main-belt asteroids with diameters >40 km using the Keck II Adaptive Optics (AO) facility. Five of these (45 Eugenia, 87 Sylvia, 107 Camilla, 121 Hermione, 130 Elektra) were confirmed to have satellite. Assuming the same albedo as the primary, these moonlets are relatively small (∼5% of the primary size) suggesting that they are fragments captured after a disruptive collision of a parent body or captured ejecta due to an impact. For each asteroid, we have estimated the minimum size of a moonlet that can positively detected within the Hill sphere of the system by estimating and modeling a 2-σ detection profile: in average on the data set, a moonlet located at 2/100 × R Hill (1/4 × R Hill ) with a diameter larger than 6 km (4 km) would have been unambiguously seen. The apparent size and shape of each asteroid was estimated after deconvolution using a new algorithm called AIDA. The mean diameter for the majority of asteroids is in good agreement with IRAS radiometric measurements, though for asteroids with a D < 200 km, it is underestimated on average by 6-8%. Most asteroids had a size ratio that was very close to those determined by lightcurve measurements. One observation of 104 Klymene suggests it has a bifurcated shape. The bi-lobed shape of 121 Hermione described in Marchis et al. [Marchis, F., Hestroffer, D., Descamps, P., Berthier, J., Laver, C., de Pater, I., 2005c. Icarus 178, 450-464] was confirmed after deconvolution. The ratio of contact binaries in our survey, which is limited to asteroids larger than 40 km, is surprisingly high (∼6%), suggesting that a non-single configuration is common in the main-belt. Several asteroids have been analyzed with lightcurve inversions. We compared lightcurve inversion models for plane-of-sky predictions with the observed images (9 Metis, 52 Europa, 87 Sylvia, 130 Elektra, 192 Nausikaa, and 423 Diotima, 511 Davida). The AO images allowed us to determine a unique photometric mirror pole solution, which is normally ambiguous for asteroids moving close to the plane of the ecliptic (e.g., 192 Nausikaa and 52 Europa). The photometric inversion models agree well with the AO images, thus confirming the validity of both the lightcurve inversion method and the AO image reduction technique.

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Section: Resultssupporting

confidence: 85%

Section: Klymenesupporting

confidence: 79%

Section: Search For Moonlet Companionsmentioning

confidence: 99%

Section: Other Asteroidsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Shape, size and multiplicity of main-belt asteroidsI. Keck Adaptive Optics survey

Marchis

Kaasalainen

Hom

et al. 2006

Icarus

109

101

View full text Add to dashboard Cite

show abstract

4.3.1 The asteroids

Harris¹

2009

Solar System

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Analysis of the potential field and equilibrium points of irregular-shaped minor celestial bodies

Wang

Jiang

Gong

2014

Astrophys Space Sci

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Abstract. The equilibrium points of the gravitational potential field of minor celestial bodies, including asteroids, comets, and irregular satellites of planets, are studied. In order to understand better the orbital dynamics of massless particles moving near celestial minor bodies and their internal structure, both internal and external equilibrium points of the potential field of the body are analyzed. In this paper, the location and stability of the equilibrium points of 23 minor celestial bodies are presented. In addition, the contour plots of the gravitational effective potential of these minor bodies are used to point out the differences between them. Furthermore, stability and topological classifications of equilibrium points are discussed, which clearly illustrate the topological structure near the equilibrium points and help to have an insight into the orbital dynamics around the irregular-shaped minor celestial bodies.The results obtained here show that there is at least one equilibrium point in the potential field of a minor celestial body, and the number of equilibrium points could be one, five, seven, and nine, which are all odd integers. It is found that for some irregular-shaped celestial bodies, there are more than four equilibrium points outside the bodies while for some others there are no external equilibrium points. If a celestial 2 body has one equilibrium point inside the body, this one is more likely linearly stable.

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Mass and density of Asteroid 121 Hermione from an analysis of its companion orbit

Cited by 38 publications

References 27 publications

Shape, size and multiplicity of main-belt asteroidsI. Keck Adaptive Optics survey

Shape, size and multiplicity of main-belt asteroidsI. Keck Adaptive Optics survey

4.3.1 The asteroids

Analysis of the potential field and equilibrium points of irregular-shaped minor celestial bodies

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