Potentially habitable flow-like features from Martian dry ice geyser dune spots

These intriguing high latitude features are associated with the Martian Geysers. The geysers themselves (if that is what they are) are thought to be results of dry ice turning to gas, and the dark spots and flow like features are thought to be debris from the geysers.

However, later in the year the flow like features extend further down the slopes. The details differ for the two hemispheres. In the Southern hemisphere, all current models for this part of the process involve liquid water. In the northern hemisphere then most of the models also involve water, although the northern hemisphere flow like features form at much lower surface temperatures.

This image shows the flow like features of the southern hemisphere.

Flow-like features in Dunes on Richardson Crater, Mars. They form around the dark dune spots, in the debris of the hypothesized Martian Geysers. The dark material at the end of the flows moves at between 0.1 and 1.4 m/day in late spring / summer on Mars. All current models for it favour liquid water as a cause. Either interfacial layers, or else layers of water created through the solid state greenhouse effect.

The process starts with the dark dune spots which form in early spring. Here are some examples in Richardson Crater in the Martian southern hemisphere- one of the places where the Flow Like Features (FLFs) have been observed.

These are thought to result from the Martian Geysers.

The idea is that a semi-transparent solid such as dry ice or clear ice acts like a greenhouse to warm up a layer below the surface (the "solid state greenhouse effect"). When this lower layer consists of dry ice, then it turns into gas and as the pressure builds up, eventually escapes to the surface explosively as a Martian Geyser.

The debris from these geysers form the dark spots, and the "flow like features".

Then, as local summer approaches, the flow like features start to extend down the slope. These are small features only a few tens of meters in scale, and grow at a rate of a meter or a few meters per Martian sol through the late Martian spring and summer. This is the part of the process that is thought to be due to liquid water, in nearly all the models proposed for them so far.

A different mechanism is proposed for them in the Northern and in the Southern hemispheres.

Solid state greenhouse effect model

Möhlmann uses a solid state greenhouse effect in his model, similarly to the process that forms the geysers, but with translucent ice rather than dry ice as the solid state greenhouse layer.

Blue wall of an Iceberg on Jökulsárlón, Iceland. On the Earth, Blue ice like this forms as a result of air bubbles squeezed out of glacier ice. This has the right optical and thermal properties to act as a solid state greenhouse, trapping a layer of liquid water that forms 0.1 to 1 meters below the surface. In Möhlmann's model, if ice with similar optical and thermal properties forms on Mars, it could form a layer of liquid water centimeters to decimeters thick, which would form 5 - 10 cm below the surface.

In his model, first the ice forms a translucent layer - then as summer approaches, the solid state greenhouse effect raises the temperature of a layer below the surface to 0 °C, so melting it. This is a process familiar on the Earth for instance in Antarctica. On Earth, in similar conditions, the surface ice remains frozen, but a layer of liquid water forms from 0.1 to 1 meters below the surface. It forms preferentially in "blue ice".

On Mars, in his model, the melting layer is 5 to 10 cm below the surface. The liquid water layer starts off millimeters thick in their model, and can develop to be centimeters thick as the season progresses. The effect of the warming is cumulative over successive sols. Once formed, the liquid layer can persist overnight. Subsurface liquid water layers like this can form with surface temperatures as low as -56 °C.

If the ice covers a heat absorbing layer at the right depth, the melted layer can form more rapidly, within a single sol, and can evolve to be tens of centimeters in thickness. In their model this starts as fresh water, insulated from the surface conditions by the overlaying ice layers - and then mixes with any salts to produce salty brines which would then flow beyond the edges to form the extending dark edges of the flow like features.

Later in the year, pressure can build up and cause formation of mini water geysers which may possibly explain the "white collars" that form around the flow like features towards the end of the season - in their model this is the result of liquid water erupting in mini water geysers and then freezing as white pure water ice.

This provides:

• A way for pure water to be present on Mars, and to stay liquid under pressure, insulated from the surface conditions.
• 5 to 10 cm below the surface, trapped by the ice above it
• Depending on conditions, the liquid layer is at least centimeters in thickness, and could be tens of centimeters in thickness.
• Initially of fresh water, at around 0 °C.

If salt grains are present in the ice, then this gives conditions for brines to form, which would increase the melt volume and the duration of the melting. The brines then flow down the slope and extend the dark patch formed by the debris from the Geyser, so creating the extensions of the flow like features.

They mention a couple of caveats for their model, because the surface conditions on Mars at these locations is unknown. First it requires conditions for bare and optically transparent ice fields on Mars translucent to depths of several centimeters, and it is an open question whether this can happen, but there is nothing to rule it out either. Then, the other open question is whether their assumption of low thermal conductivity of the ice, preventing escape of the heat to the surface, is valid on Mars. The process works with blue ice on Earth - but we can't say yet what forms the ice actually takes in these Martian conditions.

This solid state greenhouse effect process favours equator facing slopes. Also, somewhat paradoxically, it favours higher latitudes, close to the poles, over lower latitudes, because it needs conditions where surface ice can form on Mars to thicknesses of tens of centimeters. (The examples at Richardson crater are at latitude -72°, longitude 179.4°, so only 18° from the south pole.).

There is no in situ data yet for these locations, of course, to test the hypothesis. Though some of the predictions for their model could be confirmed by satellite observations.

Interfacial liquid layers model

Another model for these southern hemisphere features involves ULI water (undercooled liquid water) which forms as a thin layer over surfaces and can melt at well below the usual melting point of ice. In Mohlmann's sandwich model, then the interfacial water layer forms on the surfaces of solar heated grains in the ice, which then flows together down the slope. Calculations of downward flow of water shows that several litres a day of water could be supplied to the seepage flows in this way.

The idea then is that this ULI water would be the water source for liquid brines which then flow down the surface to form the features.

Northern Hemisphere flow like features

Seasonal processes in the Northern polar dunes with Flow Like Features. Time differences between the images are 22 days and 12 days. The final picture shows a long feature that formed new between the two images, and its length is 60 meters so it grew at a rate of at least 5 meters per day.

These features form at a much lower temperature than the southern hemisphere flow like features, at -90°C average surface temperature on kilometers scale - though the dark features are expected to be considerably warmer, and the subsurface is also expected to be heated by the solid state greenhouse effect through surface layers of dry ice (similarly to the proposed models for the Martian Geysers).

They progress through a sequence of changes, first wind blown, and then seepage features associated with the dune spots, and then finally, dark seepage features appear all along the dune crest as in this sequence. These images show the growth of the seepage features.

The flow like features in the northern hemisphere polar ice cap form at average surface temperatures of around 150°K - 180°K, i.e. up to -90 °C approximately.

The flows start as wind-blown features but then are followed by seepage features which increase at between 0.3 meters and 7 meters a day.

"They show a characteristic sequence of changes: first only wind-blown features emanate from them, while later a bright circular and elevated ring forms, and dark seepage-features start from the spots. These streaks grow with a speed between 0.3 meters per day and 7 meters per day, first only from the spots, later from all along the dune crest."

The seepage features first form at overall surface temperatures of 160°K (-110 °C), as measured with the low resolution TES data. However this has a resolution of 3 km across track and only 9 km along the track of the observations. Also, much of the area is still covered in dry ice at this point, and it is opaque in the thermal infrared band so the orbital photographs measure the temperature of the surface of the dry ice rather than the small area of the dark spots and streaks.

Then, as with the model for the Martian geysers, shortwave radiation can penetrate translucent CO₂ ice layer, and heat the subsurface through the solid state greenhouse effect.

The models suggest that subsurface melt water layers, and interfacial water could form with surface temperatures as low as 180°K (-90 °C). Salts in contact with them could then form liquid brines.

An alternative mechanism for the Northern hemisphere involves dry ice and sand cascading down the slope but most of the models involve liquid brines for the seepage stages of the features.

For details see the Dark Dune Spots section of Nilton Renno's paper which also has images of the two types of feature as they progress through the season.