Abstract
AbstractAlthough ice fracturing and deformation is key to understanding some of the landforms encountered in the high‐latitude regions on Mars and on other icy bodies in the solar system, little is known about the mechanical characteristics of CO ice. We have measured the hardness of solid CO ice directly in the laboratory with a Leeb hardness tester and calculated the corresponding yield strength. We have also measured the hardness of water ice by the same method, confirming previous work. Our results indicate that CO ice is slightly weaker, ranging between Leeb 200 and 400 ( 10 and 30 MPa yield strength, assuming only plastic deformation and no strain hardening during the experiment), for typical Martian temperatures. Our results can be used for models of CO ice rupture (depending on the deformation timescales) explaining surface processes on Mars and solar system icy bodies.
Highlights
The surfaces of numerous solar system bodies are wholly or partly covered with water and/or carbon dioxide ice whose dynamics play a key role in the shaping of planetary landforms
We have measured the hardness of solid CO2 ice directly in the laboratory with a Leeb hardness tester and calculated the corresponding yield strength
Our results indicate that CO2 ice is slightly weaker, ranging between Leeb ∼200 and 400 (∼10 and 30 MPa yield strength, assuming only plastic deformation and no strain hardening during the experiment), for typical Martian temperatures
Summary
The surfaces of numerous solar system bodies are wholly or partly covered with water and/or carbon dioxide ice whose dynamics play a key role in the shaping of planetary landforms. Quantifying the dynamic behavior of CO2 ice is important to address questions relating to the processes resulting in araneiforms. These are channel-like features scoured in the polar regolith by hypothesized gas flow under a layer of CO2 ice (Kieffer, 2007). When this gas pressure exceeds the—unknown—rupture strength of the overlying ice, gas and regolith can be ejected onto the surface, creating plumes and playing an important role in dust transportation on Mars. Beyond Mars, understanding the strength of CO2 ice is relevant to the mechanical properties of icy regoliths on the surfaces and interiors of outer solar system objects such as comets and Kuiper belt objects
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