Recent liquid water flow on Mars has been proposed based on geomorphological features,
such as gullies. Recurring slope lineae—seasonal flows that are darker than their …

Extensive evidence of landform-scale martian geomorphic changes has been acquired in
the last decade, and the number and range of examples of surface activity have increased …

Exploring the subsurface structure and stratification of Mars advances our understanding of
Martian geology, hydrological evolution and palaeoclimatic changes, and has been a main …

Water is a requirement for life as we know it. Indirect evidence of transient liquid water has
been observed from orbiter on equatorial Mars, in contrast with expectations from large …

Water probably flowed across ancient Mars, but whether it ever exists as a liquid on the
surface today remains debatable. Recurring slope lineae (RSL) are narrow (0.5 to 5 meters) …

This chapter focuses almost exclusively on marine evaporites and in particular on how the
chemistry of seawater is reflected in the mineralogy and facies distribution of deposits in …

Carbonate minerals are of particular interest in paleoenvironmental research as they are an
integral part of the carbon and water cycles, both of which are relevant to habitability. Given …

Liquid water is a basic ingredient for life as we know it. Therefore, in order to understand the
habitability of other planets we must first understand the behavior of water on them. Mars is …

Salt solutions on Mars can stabilize liquid water at low temperatures by lowering the freezing
point of water. The maximum equilibrium freezing-point depression possible, known as the …

Volcanic outgassing is one of the main sources of volatiles for the martian atmosphere and
degassing of the martian interior potentially influenced the early martian climate. Using a …