Groove formation on Phobos: Testing the Stickney ejecta emplacement model for a subset of the groove population

@article{Wilson2015GrooveFO,
  title={Groove formation on Phobos: Testing the Stickney ejecta emplacement model for a subset of the groove population},
  author={Lionel Wilson and James W. Head},
  journal={Planetary and Space Science},
  year={2015},
  volume={105},
  pages={26-42}
}
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References

SHOWING 1-10 OF 100 REFERENCES
Martian impacts and the grooves of Phobos: implications for the evolution of Phobos' rotation axis
Recent work has suggested that the grooves of Phobos might be explained as chains of coalesced secondary craters from impacts on Mars [1,2]. This work examined groove characteristics and orientations
Grooves on Phobos: Their distribution, morphology and possible origin
A remarkable characteristic of the surface of Phobos is that it is densely covered by grooves—long linear depressions formed in a regolith. Typically, grooves are 100–200 m wide, 10–20 m deep, and
Impact fracture patterns on phobos ellipsoids
Drainage pits in cohesionless materials: implications for surface of Phobos.
TLDR
These experiments indicate that the Phobos grooves and pits formed as drainage structures are the surface traces of fractures in the underlying solid body of Phobos.
The origin of grooves and crater chains of Phobos
A. Most crater chains strongly resemble secondary impact craters in their morphology. B. Groove and chain configurations consist of the intersections of planes with the surface of Phobos. C.
Ejecta Emplacement on the Martian Satellites
Abstract Ejecta features on the martian satellites are compared to models of ballistic emplacement and downslope motion. The asymmetric distribution of ejecta around the large crater Stickney on
Morphological and geographical evidence for the origin of Phobos' grooves from HRSC Mars Express images
Abstract The surface of Phobos, the 27×22×18 km inner moon of Mars, is dominated by several families of parallel grooves. At least seven different groups of hypotheses have been advanced to explain
The Stickney Impact of Phobos: A Dynamical Model
Abstract Phobos, the largest moon of Mars, has dimensions typical of minor asteroids, approximately 19 × 22 × 27 km. It is probably the best studied small planetary body in the Solar System, imaged
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