JpGU-AGU Joint Meeting 2017

Presentation information

[EJ] Oral

P (Space and Planetary Sciences) » P-PS Planetary Sciences

[P-PS05] [EJ] Mars and Mars system: results from a broad spectrum of Mars studies and aspects for future missions

Sat. May 20, 2017 3:30 PM - 5:00 PM Convention Hall B (International Conference Hall 2F)

convener:Hideaki Miyamoto(University of Tokyo), Tomohiro Usui(Earth-Life Science Institute, Tokyo Institute of Technology ), Ayako Matsuoka(Research Division for Space Plasma, Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency), Sushil K Atreya(University of Michigan Ann Arbor), Chairperson:Tomohiro Usui(Earth-Life Science Institute, Tokyo Institute of Technology ), Chairperson:Hideaki Miyamoto(University of Tokyo)

4:30 PM - 4:45 PM

[PPS05-11] Grooves on Phobos: Results of repetitious impacts of aligned fragments

*Hiroshi Kikuchi1, Hideaki Miyamoto1 (1.The University of Tokyo)

Keywords:Phobos, Groove

Numerous lineaments (grooves) are found on Phobos, but not on Deimos. This might be important to understand the origin and surface evolution of these Martian satellites. Several formation processes of grooves on Phobos have been hypothesized and discussed for years (1-4). However, none of these hypothesized processes can successfully explain the difference in surface expression between the two satellites, which includes the grooves on Phobos and the relatively smooth surface on Deimos.
In this comprehensive investigation, we mapped the grooves by using thousands of images of Phobos to plot each groove on a numerical shape model in order to accurately determine their distribution patterns. We found that all of the identified grooves exist on the corresponding planes, and they could be divided into five trends. This result indicates that the grooves are not due to collapse of the surface of Phobos. We, instead, propose that these depressions are the result of impacts by chains of projectiles; a small body with a rubble-pile structure held together by self-gravity could be pulled apart and stretched into an alignment by tides during the body’s close approach to Mars.
Through computer simulations using a N-body numerical code and scaling law, the patterns of pit chains consistent with those observed in the images of Phobos can only be produced when the stretched rubble-pile body orbits about Mars. The effect of the orbital precession of the impactor can explain the five trends. Furthermore, the deficiency of grooves can be explained by this model. Consistent with this hypothesized mode of formation of the observed grooves, intersection of Phobos with impactor composed of < 10 m-diameter fragments can also explain their origin.

1. T. A. Hurford et al., Tidal disruption of Phobos as the cause of surface fractures. Journal of Geophysical Research-Planets 121, 1054-1065 (2016).
2. H. Kikuchi, H. Miyamoto, in Lunar and Planetary Science Conference. (2014), vol. 45, pp. 2007.
3. J. B. Murray, D. C. Heggie, Character and origin of Phobos' grooves. Planetary and Space Science 102, 119-143 (2014).
4. M. Nayak, E. Asphaug, Sesquinary catenae on the Martian satellite Phobos from reaccretion of escaping ejecta. Nature Communications 7, (2016).