Hostname: page-component-78c5997874-j824f Total loading time: 0 Render date: 2024-11-02T21:50:08.646Z Has data issue: false hasContentIssue false
  • English
  • Français

The distribution and source of boulders on asteroid 4179 Toutatis

Published online by Cambridge University Press:  01 March 2016

Yun Jiang ,
Jianghui Ji ,
Jiangchuan Huang ,
Simone Marchi ,
Yuan Li  and
Wing-Huen Ip
Yun Jiang
Affiliation:
Key Laboratory of Planetary Sciences, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China email: [email protected]; [email protected]
Jianghui Ji
Affiliation:
Key Laboratory of Planetary Sciences, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China email: [email protected]; [email protected]
Jiangchuan Huang
Affiliation:
China Academy of Space Technology, Beijing 100094, China
Simone Marchi
Affiliation:
Southwest Research Institute, Boulder, Colorado 80302, USA
Yuan Li
Affiliation:
Space Science Institute, Macau University of Science and Technology, Taipa, Macau
Wing-Huen Ip
Affiliation:
Institute of Astronomy, National Central University, Taoyuan, Taiwan
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Boulders are ubiquitous on the surfaces of asteroids and their spatial and size distributions provide information for the geological evolution and collisional history of parent bodies. We identify more than 200 boulders on near-Earth asteroid 4179 Toutatis based on images obtained by Chang'e-2 flyby. The cumulative boulder size frequency distribution (SFD) gives a power-index of −4.4 ± 0.1, which is clearly steeper than those of boulders on Itokawa and Eros, indicating much high degree of fragmentation. Correlation analyses with craters suggest that most boulders cannot solely be produced as products of cratering, but are probably survived fragments from the parent body of Toutatis, accreted after its breakup. Similar to Itokawa, Toutatis probably has a rubble-pile structure, but owns a different preservation state of boulders.

Keywords

Minor planetsasteroidsplanets and satellites: individual (4179 Toutatis)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Issue S318: Asteroids: New Observations, New Models , August 2015 , pp. 153 - 155
Copyright
Copyright © International Astronomical Union 2016 

References

Busch, M. W.et al. 2012, 2012 AGU Fall Meeting, P31A-1873Google Scholar
Fujiwara, A.et al. 2006, Science, 312, 1330Google Scholar
Huang, J. C.et al. 2013, Scientific Reports, 3, 3411CrossRefGoogle Scholar
Hudson, R. S., Ostro, S. J., & Scheeres, D. J. 2003, Icarus, 161, 346CrossRefGoogle Scholar
Ji, J. H., Jiang, Y., Zhao, Y. H., Wang, S., & Yu, L. L. 2016, this volumeGoogle Scholar
Jiang, Y., Ji, J. H., Huang, J. C., Marchi, S., Li, Y., & Ip, W.-H. 2015, Scientific Reports, 5, 16029Google Scholar
Lee, P.et al. 1996, Icarus, 120, 87Google Scholar
Mazrouei, S., Daly, M. G., Barnouin, O. S., Ernst, C. M., & DeSouza, I. 2014, Icarus, 229, 181CrossRefGoogle Scholar
Thomas, P. C., Veverka, J., Robinson, M. S., & Murchie, S. 2001, Nature, 413, 394CrossRefGoogle Scholar
Zhao, Y. H.et al. 2015, MNRAS, 450, 3620Google Scholar
Zhu, M. H.et al. 2014, Geophys. Res. Lett., 41, 328Google Scholar
Zou, X.et al. 2014, Icarus, 229, 348Google Scholar