Advertisement

Results: Shapes of Impact Outcomes

  • Keisuke SugiuraEmail author
Chapter
  • 6 Downloads
Part of the Springer Theses book series (Springer Theses)

Abstract

In this chapter, we introduce the results of our simulations that investigate shapes of asteroids formed through various collisions between asteroids. Database of Asteroid Models from Inversion Techniques provides almost all shapes of known asteroids with diameters larger than 100 km. Thus, in our impact simulations, we set radius of target asteroids to 50 km to allow us to directly compare the results of our simulations with the shapes of actual asteroids. We vary impact angles, impact velocities, and ratios of the mass of impactor asteroids to that of target asteroids, and we conduct various impact simulations. As a result, we find that similar-mass and low-velocity impacts produce various shapes including extremely flat and elongated shapes. In contrast, high-velocity and destructive impacts mainly produce spherical and bilobed shapes, but they are difficult to produce flat shapes.

Keywords

Numerical simulations Collisions between asteroids Shapes of collisional outcomes 

References

  1. C. Agnor, E. Asphaug, Accretion efficiency during planetary collisions. Astrophys. J. 613, L157–L160 (2004). https://doi.org/10.1086/425158
  2. E. Asphaug, Similar-sized collisions and the diversity of planets. Chem. Erde. Geochem. 70, 199–219 (2010).  https://doi.org/10.1016/j.chemer.2010.01.004
  3. A. Fujiwara, G. Kamimoto, A. Tsukamoto, Expected shape distribution of asteroids obtained from laboratory impact experiments. Nature 272, 602 (1978).  https://doi.org/10.1038/272602a0
  4. A. Fujiwara, J. Kawaguchi, D.K. Yeomans, M. Abe, T. Mukai, T. Okada, J. Saito, H. Yano, M. Yoshikawa, D.J. Scheeres, O. Barnouin-Jha, A.F. Cheng, H. Demura, R.W. Gaskell, N. Hirata, H. Ikeda, T. Kominato, H. Miyamoto, A.M. Nakamura, R. Nakamura, S. Sasaki, K. Uesugi, The rubble-pile asteroid Itokawa as observed by Hayabusa. Science 312, 1330–1334 (2006).  https://doi.org/10.1126/science.1125841CrossRefADSGoogle Scholar
  5. G.H. Heiken, D.T. Vaniman, B.M. French, Lunar Sourcebook—A User’s Guide to the Moon (1991)Google Scholar
  6. J.P. Huchra, M.J. Geller, Groups of galaxies. I—Nearby groups. Astrophys. J. 257, 423–437 (1982).  https://doi.org/10.1086/160000
  7. Z.M. Leinhardt, S.T. Stewart, Collisions between gravity-dominated bodies. I. Outcome regimes and scaling laws. Astrophys. J. 745, 79 (2012).  https://doi.org/10.1088/0004-637X/745/1/79
  8. T. Michikami, T. Kadokawa, A. Tsuchiyama, A. Hagermann, T. Nakano, K. Uesugi, S. Hasegawa, Influence of petrographic textures on the shapes of impact experiment fine fragments measuring several tens of microns: comparison with Itokawa regolith particles. Icarus 302, 109–125 (2018).  https://doi.org/10.1016/j.icarus.2017.10.040CrossRefADSGoogle Scholar
  9. S.R. Schwartz, P. Michel, M. Jutzi, S. Marchi, Y. Zhang, D.C. Richardson, Catastrophic disruptions as the origin of bilobate comets. Nat. Astron. 2, 379–382 (2018).  https://doi.org/10.1038/s41550-018-0395-2
  10. K. Sugiura, H. Kobayashi, S. Inutsuka, Toward understanding the origin of asteroid geometries. Variety in shapes produced by equal-mass impacts. Astron. Astrophys. 620, A167 (2018).  https://doi.org/10.1051/0004-6361/201833227
  11. K. Sugiura, H. Kobayashi, S. Inutsuka, High-resolution simulations of catastrophic disruptions: resultant shape distributions. Planet. Space Sci. 181, 104807 (2020).  https://doi.org/10.1016/j.pss.2019.104807

Copyright information

© Springer Nature Singapore Pte Ltd. 2020

Authors and Affiliations

  1. 1.Earth-Life Science InstituteTokyo Institute of TechnologyMeguroJapan

Personalised recommendations