Dust Devil Tracks

Dust devils that leave dark- or light-toned tracks are common on Mars and they can also be found on the Earth’s surface. Dust devil tracks (hereinafter DDTs) are ephemeral surface features with mostly sub-annual lifetimes. Regarding their size, DDT widths can range between ∼1 m and ∼1 km, depending on the diameter of dust devil that created the track, and DDT lengths range from a few tens of meters to several kilometers, limited by the duration and horizontal ground speed of dust devils. DDTs can be classified into three main types based on their morphology and albedo in contrast to their surroundings; all are found on both planets: (a) dark continuous DDTs, (b) dark cycloidal DDTs, and (c) bright DDTs. Dark continuous DDTs are the most common type on Mars. They are characterized by their relatively homogenous and continuous low albedo surface tracks. Based on terrestrial and martian in situ studies, these DDTs most likely form when surficial dust layers are removed to expose larger-grained substrate material (coarse sands of ≥500 μm in diameter). The exposure of larger-grained materials changes the photometric properties of the surface; hence leading to lower albedo tracks because grain size is photometrically inversely proportional to the surface reflectance. However, although not observed so far, compositional differences (i.e., color differences) might also lead to albedo contrasts when dust is removed to expose substrate materials with mineralogical differences. For dark continuous DDTs, albedo drop measurements are around 2.5 % in the wavelength range of 550–850 nm on Mars and around 0.5 % in the wavelength range from 300–1100 nm on Earth. The removal of an equivalent layer thickness around 1 μm is sufficient for the formation of visible dark continuous DDTs on Mars and Earth. The next type of DDTs, dark cycloidal DDTs, are characterized by their low albedo pattern of overlapping scallops. Terrestrial in situ studies imply that they are formed when sand-sized material that is eroded from the outer vortex area of a dust devil is redeposited in annular patterns in the central vortex region. This type of DDT can also be found in on Mars in orbital image data, and although in situ studies are lacking, terrestrial analog studies, laboratory work, and numerical modeling suggest they have the same formation mechanism as those on Earth. Finally, bright DDTs are characterized by their continuous track pattern and high albedo compared to their undisturbed surroundings. They are found on both planets, but to date they have only been analyzed in situ on Earth. Here, the destruction of aggregates of dust, silt and sand by dust devils leads to smooth surfaces in contrast to the undisturbed rough surfaces surrounding the track. The resulting change in photometric properties occurs because the smoother surfaces have a higher reflectance compared to the surrounding rough surface, leading to bright DDTs. On Mars, the destruction of surficial dust-aggregates may also lead to bright DDTs. However, higher reflective surfaces may be produced by other formation mechanisms, such as dust compaction by passing dust devils, as this may also cause changes in photometric properties. On Mars, DDTs in general are found at all elevations and on a global scale, except on the permanent polar caps. DDT maximum areal densities occur during spring and summer in both hemispheres produced by an increase in dust devil activity caused by maximum insolation. Regionally, dust devil densities vary spatially likely controlled by changes in dust cover thicknesses and substrate materials. This variability makes it difficult to infer dust devil activity from DDT frequencies. Furthermore, only a fraction of dust devils leave tracks. However, DDTs can be used as proxies for dust devil lifetimes and wind directions and speeds, and they can also be used to predict lander or rover solar panel clearing events. Overall, the high DDT frequency in many areas on Mars leads to drastic albedo changes that affect large-scale weather patterns

Climate and Land Degradation

On the occasion of the Seventh session of the Conference of Parties, The World Meteorological Organization (WMO) has prepared this brochure which explains the role of different climatic factors in land degradation and WMO's contribution in addressing this important subject. Educational levels: Undergraduate lower division, Undergraduate upper division, Graduate or professional, Informal education, General public

Proceedings of the Polar Processes on Mars Workshop

Included in this publication is a collection of abstracts from the NASA-sponsored workshop, Polar Processes on Mars, which was held at the Sunnyvale Hilton Hotel, Sunnyvale, California, on 12 to 13 May 1988. Support for the workshop came from NASA's Planetary Geology and Geophysics program managed by Dr. Jospeh Boyce. The workshop is one of a series identified by MECA (an acronym for Mars: Evolution of its Climate and Atmosphere) as being worthy of focused research, but one for which it was not possible to hold during the project's lifetime. Consequently, it was held after the project ended. The MECA project was part of the Mars Data Analysis program. The workshop consisted of four sessions: The Polar Caps, Dynamics/Atmospheric Processes, Polar Geology, and Future Measurements. To put things into perspective, each of the first three sessions began with a review. All sessions were scheduled to allow ample time for discussion. A brief review of each session is provided

High-Resolution Martian Soil Thickness Derived from Yearly Surface Temperatures

abstract: The temperature of a planet's surface depends on numerous physical factors, including thermal inertia, albedo and the degree of insolation. Mars is a good target for thermal measurements because the low atmospheric pressure combined with the extreme dryness results in a surface dominated by large differences in thermal inertia, minimizing the effect of other physical properties. Since heat is propagated into the surface during the day and re-radiated at night, surface temperatures are affected by sub-surface properties down to several thermal skin depths. Because of this, orbital surface temperature measurements combined with a computational thermal model can be used to determine sub-surface structure. This technique has previously been applied to estimate the thickness and thermal inertia of soil layers on Mars on a regional scale, but the Mars Odyssey Thermal Emission Imaging System "THEMIS" instrument allows much higher-resolution thermal imagery to be obtained. Using archived THEMIS data and the KRC thermal model, a process has been developed for creating high-resolution maps of Martian soil layer thickness and thermal inertia, allowing investigation of the distribution of dust and sand at a scale of 100 m/pixel.Dissertation/ThesisM.S. Geological Sciences 201

Desertification

IPCC SPECIAL REPORT ON CLIMATE CHANGE AND LAND (SRCCL) Chapter 3: Climate Change and Land: An IPCC special report on climate change, desertification, land degradation, sustainable land management, food security, and greenhouse gas fluxes in terrestrial ecosystem

Mechanistic Contributions To Geomorphic Changes Of State

Transitions abound in geomorphology. Be it the transition from static to dynamic or the shift in a dune field from one dune morphology to another, many questions involve changes of state. This dissertation empirically studies state changes over three scales with an emphasis placed on contributing mechanical factors. First, we examine the transition from static to dynamic at the grain scale in bedload transport (hopping, rolling, and skipping of grains along a riverbed). Transport of grains is continuous at high rates but becomes unpredictable near the threshold of motion. Results show that this unpredictability is similar to how avalanches occur in a sandpile. Transport events are similar in size and merge as transport increases. Grain displacement in the system appears governed by mobile grain-bed kinetic energy exchange. Next, we study the static to dynamic transition at the scale of many grains by examining how soil mechanical properties influence the threshold of motion. Sandbed experiments indicate that, when moisture is the primary variable, shear strength is proportional to the threshold of motion. Finally, we examine a landscape scale pattern transition that arises from the physics of sediment transport interacting with vegetation in a dune field. The onset of vegetation destroys a fluid instability that is fundamental for maintaining the dune pattern prevalent in the dune fields center. Plants destroy the mechanism maintaining the dune field pattern which helps give rise to a qualitative shift in dune morphology. This work highlights the continued relevance of physically informed experiments and field studies for understanding geomorphic transitions from the grain to the landscape scale