Imperial College London

Professor Gareth Collins

Faculty of EngineeringDepartment of Earth Science & Engineering

Professor of Planetary Science



+44 (0)20 7594 1518g.collins Website




4.83Royal School of MinesSouth Kensington Campus






BibTex format

author = {Brooker, LM and Balme, MR and Conway, SJ and Hagermann, A and Barrett, AM and Collins, GS and Soare, RJ},
doi = {10.1016/j.icarus.2017.11.022},
journal = {Icarus},
pages = {386--406},
title = {Clastic polygonal networks around Lyot crater, Mars: Possible formation mechanisms from morphometric analysis},
url = {},
volume = {302},
year = {2017}

RIS format (EndNote, RefMan)

AB - Polygonal networks of patterned ground are a common feature in cold-climate environments. They can form through the thermal contraction of ice-cemented sediment (i.e. formed from fractures), or the freezing and thawing of ground ice (i.e. formed by patterns of clasts, or ground deformation). The characteristics of these landforms provide information about environmental conditions. Analogous polygonal forms have been observed on Mars leading to inferences about environmental conditions. We have identified clastic polygonal features located around Lyot crater, Mars (50°N, 30°E). These polygons are unusually large ( > 100 m diameter) compared to terrestrial clastic polygons, and contain very large clasts, some of which are up to 15 metres in diameter. The polygons are distributed in a wide arc around the eastern side of Lyot crater, at a consistent distance from the crater rim. Using high-resolution imaging data, we digitised these features to extract morphological information. These data are compared to existing terrestrial and Martian polygon data to look for similarities and differences and to inform hypotheses concerning possible formation mechanisms. Our results show the clastic polygons do not have any morphometric features that indicate they are similar to terrestrial sorted, clastic polygons formed by freeze-thaw processes. They are too large, do not show the expected variation in form with slope, and have clasts that do not scale in size with polygon diameter. However, the clastic networks are similar in network morphology to thermal contraction cracks, and there is a potential direct Martian analogue in a sub-type of thermal contraction polygons located in Utopia Planitia. Based upon our observations, we reject the hypothesis that polygons located around Lyot formed as freeze-thaw polygons and instead an alternative mechanism is put forward: they result from the infilling of earlier thermal contraction cracks by wind-blown material, which then beca
AU - Brooker,LM
AU - Balme,MR
AU - Conway,SJ
AU - Hagermann,A
AU - Barrett,AM
AU - Collins,GS
AU - Soare,RJ
DO - 10.1016/j.icarus.2017.11.022
EP - 406
PY - 2017///
SN - 0019-1035
SP - 386
TI - Clastic polygonal networks around Lyot crater, Mars: Possible formation mechanisms from morphometric analysis
T2 - Icarus
UR -
UR -
VL - 302
ER -