Speaker
Description
This presentation introduces a theoretical model that explores the
possibilities of how liquid water could persist on the surface of
Mars. Indeed, hygroscopic salt crystals found on the surface are
capable of binding atmospheric water vapor, thereby forming a liquid
solution. The main challenge is preserving these solutions in the
extremely dry daytime environment. The model is based on volume
changes caused by significant daily temperature fluctuations, which
generate internal stress and can cause cracks to form in the salt crystals.
As a result of low evening temperatures and the concomitant increase
in relative humidity, the deliquescent liquid can flow into an
internal cavity of the crystal; then, as the temperature rises during the day, the
cracks may close, thereby isolating the solution from the dry outdoor
environment. Based on a simulation run on Ca(ClO4)2 salt crystals, the
probability of liquid formation as deliquescence can reach as high as 100–130 sols on
average per year near Acidalia Planitia. An analysis of this process
reveals a strong correlation with surface thermal inertia (TI);
elucidating the underlying mechanisms could lead to a better
understanding of physical processes on Mars. To this end, a detailed
analysis of specific locations is of paramount importance to gain a
more precise insight into which factors play a role in this phenomenon
and to what extent.