Small-scale topography of 25143 Itokawa from the Hayabusa laser altimeter

Barnouin, Olivier S.; Cheng, A. F.; Mukai, T.; Abe, Shinsuke; Hirata, Naru; Nakamura, Ryosuke; Gaskell, R. W.; Saito, Junji; Clark, B. E.

doi:10.1016/j.icarus.2008.05.026

Cited by 81 publications

(95 citation statements)

References 44 publications

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“…1(a), is about 540 m along its longest axis, and is believed to be a socalled "rubble pile," formed through gravitational accretion followed by collisional and weathering processes 7 . Raised areas 2 on Itokawa are populated by boulders ranging in diameter 3,4 from 5 to 40 m, while depressions are filled with smooth seas of smaller particles 5 ranging from fine dust to centimeter-sized pebbles 6 . It is not known how this segregation came about, and understanding this may shed light on the processes that asteroids 7,8,9 -and perhaps other bodies 10,11 -undergo during formation and development.…”

Section: Doi: …mentioning

confidence: 99%

Size Sorting on the Rubble-Pile Asteroid Itokawa

et al. 2017

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Section: Doi: …mentioning

confidence: 99%

Size Sorting on the Rubble-Pile Asteroid Itokawa

et al. 2017

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“…2. Two major smooth regions that exist on Itokawa are located close to the poles (Demura et al 2006;Barnouin-Jha et al 2008). 3.…”

Section: Simplified Meshesmentioning

confidence: 99%

The YORP effect on 25 143 Itokawa

Breiter

Bartczak

Czekaj

et al. 2009

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Context. The asteroid 25143 Itokawa is one of the candidates for the detection of the Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect in the rotation period. Previous studies were carried out up to the 196 608 facets triangulation model and were not able to provide a good theoretical estimate of this effect, raising questions about the influence of the mesh resolution and the centre of mass location on the evolution the rotation period. Aims. The YORP effect on Itokawa is computed for different topography models up to the highest resolution Gaskell mesh of 3 145 728 triangular faces in an attempt to find the best possible YORP estimate. Other, lower resolution models are also studied and the question of the dependence of the rotation period drift on the density distribution inhomogeneities is reexamined. A comparison is made with 433 Eros models possessing a similar resolution. Methods. The Rubincam approximation (zero conductivity) is assumed in the numerical simulation of the YORP effect in rotation period. The mean thermal radiation torques are summed over triangular facets assuming Keplerian heliocentric motion and uniform rotation around a body-fixed axis.Results. There is no evidence of YORP convergence in Gaskell model family. Differently simplified meshes may converge quickly to their parent models, but this does not prove the quality of YORP computed from the latter. We confirm the high sensitivity of the YORP effect to the fine details of the surface for 25 143 Itokawa and 433 Eros. The sensitivity of the Itokawa YORP to the centre of mass shift is weaker than in earlier works, but instead the results prove to be sensitive to the spin axis orientation in the body frame. Conclusions. Either the sensitivity of the YORP effect is a physical phenomenon and all present predictions are questionable, or the present thermal models are too simplified.

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“…This latter result, together with images showing that its granular surface is covered by large pieces of debris, as well as simulations of catastrophic disruption and re-accumulation (Michel and Richardson, 2013), suggest that Itokawa is indeed a rubble pile (Fujiwara et al, 2006). From surface images, it seems to be composed of 100-200 m blocks and to be covered by a thin regolith mainly composed of gravels and pebbles (Barnouin-Jha et al, 2008 and Figure 1). However, each of these larger blocks can be a monolith or an aggregate of smaller blocks, pebbles or gravels, and other internal structures can be invoked to explain the same observable features.…”

Section: -1 Deep Interior and Collisional Historymentioning

confidence: 67%

“…Another scenario, which best explains binary systems consisting of a very large primary, not necessarily with a top shape, and a very small satellite is the formation of a satellite during a catastrophic disruption when the ejected debris reaccumulates and some of them become two gravitationally bound bodies (Durda et al, 2004;Michel et al, 2001). JAXA Fujiwara et al, 2006);is a candidate example of the aggregate or rubble-pile structural model (right from Barnouin-Jha et al, 2008) …”

Section: -1 Deep Interior and Collisional Historymentioning

confidence: 99%