Morphology of asteroid (4179) Toutatis as imaged by Chang'E‐2 spacecraft

Close observations by the Chang'E‐2 spacecraft reveal that the surface of asteroid (4179) Toutatis is characterized by abundant impact craters with most of them being degraded by surface resetting. The less degraded large crater with a diameter of ~800 m at the south pole is estimated to be produced by an impactor with a diameter of ~50 m from strength crater scaling relations. From the analysis of large‐impact events on highly porous targets, we argue that Toutatis is likely a rubble‐pile body and its two lobes are contact binaries. The fact that Toutatis suffered plenty of impacts with seismic shaking resetting the initial surface features but not resulting in catastrophic disruption is probably because of the material's high attenuation of shock wave.

[1]  K. Holsapple,et al.  Momentum transfer in asteroid impacts. I. Theory and scaling , 2012 .

[2]  M. Gaffey,et al.  Composition of near-Earth Asteroid (4179) Toutatis , 2012, 1210.2853.

[3]  K. Holsapple,et al.  Craters without ejecta , 2012 .

[4]  S. Debei,et al.  E-Type Asteroid (2867) Steins as Imaged by OSIRIS on Board Rosetta , 2010, Science.

[5]  A. Cheng.  Fundamentally distinct outcomes of asteroid collisional evolution and catastrophic disruption , 2009 .

[6]  K. A. Holsapple,et al.  On the ''strength'' of the small bodies of the solar system: A review of strength theories and their implementation for analyses of impact disruptions , 2009 .

[7]  E. Asphaug.  Critical crater diameter and asteroid impact seismology , 2008 .

[8]  K. Holsapple,et al.  A crater and its ejecta: An interpretation of Deep Impact , 2007 .

[9]  J. Kawaguchi,et al.  The Rubble-Pile Asteroid Itokawa as Observed by Hayabusa , 2006, Science.

[10]  P. Thomas,et al.  Seismic resurfacing by a single impact on the asteroid 433 Eros , 2005, Nature.

[11]  P. Schultz,et al.  Expectations for Crater Size and Photometric Evolution from the Deep Impact Collision , 2005 .

[12]  Richard Greenberg,et al.  Impact-Induced Seismic Activity on Asteroid 433 Eros: A Surface Modification Process , 2004, Science.

[13]  Kevin R. Housen,et al.  Impact cratering on porous asteroids , 2003 .

[14]  Daniel J. Scheeres,et al.  High-resolution model of Asteroid 4179 Toutatis , 2003 .

[15]  M. Belton,et al.  The Diagnosis of Complex Rotation in the Lightcurve of 4179 Toutatis , 2002 .

[16]  S. Murchie,et al.  Asteroid Geology from Galileo and NEAR Shoemaker Data , 2002 .

[17]  E. Dejong,et al.  Dynamics of Orbits Close to Asteroid 4179 Toutatis , 1998 .

[18]  R. Sullivan,et al.  Mechanical and geological effects of impact cratering on Ida , 1996 .

[19]  J. Head,et al.  Collisional and Dynamical History of Ida , 1996 .

[20]  Steven J. Ostro,et al.  Shape and Non-Principal Axis Spin State of Asteroid 4179 Toutatis , 1995, Science.

[21]  Martin A. Slade,et al.  Radar Images of Asteroid 4179 Toutatis , 1995, Science.

[22]  Elisabetta Dotto,et al.  The lightcurve of 4179 Toutatis: Evidence for complex rotation. , 1995 .

[23]  J. Bell,et al.  Visible and Near-Infrared Spectral Observations of 4179 Toutatis , 1994 .

[24]  A. Whipple,et al.  Long-term dynamical evolution of the minor planet (4179) Toutatis , 1993 .

[25]  G. Hahn,et al.  Dynamics of planet-crossing asteroids: Classes of orbital behavior: Project SPACEGUARD , 1989 .

[26]  J. Veverka,et al.  Grooves on asteroids: A prediction , 1979 .

[27]  Verne R. Oberbeck,et al.  Thickness determinations of the lunar surface layer from lunar impact craters. , 1968 .

[28]  N. Mcbride,et al.  Near-infrared spectra of 12 Near-Earth Objects , 2007 .

[29]  Steven J. Ostro,et al.  Asteroid 4179 Toutatis: 1996 Radar Observations , 1999 .

[30]  K. Holsapple,et al.  Compaction as the origin of the unusual craters on the asteroid Mathilde , 1999, Nature.

[31]  R. Greeley,et al.  Discovery of Grooves on Gaspra , 1994 .