Extended Abstract



Introduction

The Lut Desert in Iran, one of the hottest and most arid deserts on Earth, hosts an extensive array of yardangs, whose unique geological and climatic conditions provide an ideal natural laboratory for studying erosional processes. In contrast, the Aeolis region of Mars, extensively explored by NASA's orbiters and rovers, features yardangs that exhibit striking morphological parallels to their terrestrial counterparts in terms of shape, orientation, and erosion patterns. A comparative analysis of these two regions offers valuable insights into the influence of climatic factors, material composition, and erosional dynamics in two distinct yet analogous environments. One effective approach to investigating these phenomena is the geomorphological modeling of yardang development stages, which enables the simulation of their formation, growth, and evolutionary trajectories over time. Such modeling not only enhances our understanding of the environmental and geological drivers behind yardang evolution but also facilitates a more precise comparative framework between terrestrial and Martian analogs. In this study, geomorphological modeling techniques, including three-dimensional reconstruction, are employed to simulate the developmental stages of the Lut Desert yardangs and compare them with those in the Aeolis region of Mars. The research pursues two primary objectives: first, to identify the dominant processes governing yardang formation in the Lut Desert and on Mars, and second, to analyze the key factors influencing these processes across both planetary contexts.



Methodology

In this study, Landsat 9 satellite imagery was initially acquired via Google Earth Engine for the Lut Desert region. A digital elevation model (DEM) of the area was subsequently extracted from the United States Geological Survey (USGS) database. Following this, the yardangs within the Lut Desert were systematically identified. To evaluate these geomorphological structures and assess the role of wind in yardang formation, the DEM data were integrated into the Global Wind Atlas platform. Key parameters, including the frequency, velocity, and intensity of prevailing winds, were then computed and analyzed.

Results and Discussion

Wind Frequency, Velocity, and Power

The results revealed that the predominant wind frequency in the Lut Desert yardangs is 30%, with winds predominantly originating from the northwest. Wind velocity emerged as a critical factor in yardang formation, with 50% of measured wind speeds attributed to the dominant northwest winds in the study area. The third parameter, wind power, demonstrated that northwest winds account for 60% of the total wind energy in the Lut Desert. This high wind power underscores the significant erosional capacity of northwestern winds to modify surface features and induce substantial changes in geomorphological structures. Wind power is directly correlated with its capacity to transport and displace sedimentary particles, a process that profoundly influences yardang morphology.

Processes Driving the Genesis and Evolution of Lut Desert Yardangs

The findings indicate that the Lut Desert yardangs have evolved through the interplay of endogenic and exogenic processes. Aeolian and hydrological forces, combined with lithological variations, have generated diverse erosional patterns in the region, ultimately producing the distinct geomorphological forms of the Lut yardangs.

Developmental Stages of Lut Desert Yardangs

Analysis of the Lut Desert yardangs enabled the proposal of a five-stage developmental model. This model not only provides a comprehensive explanation of yardang evolution but also facilitates the interpretation of how factors such as wind dynamics, hydrological activity, lithology, and environmental conditions collectively shape these structures. The model assigns primary agency to aeolian processes in yardang formation and serves as a holistic framework for studying yardangs in extraterrestrial contexts, including Mars.

Analysis of Martian Yardangs

The yardangs in the Aeolis Planum region of Mars are predominantly classified as "hogback" types, characterized by rounded forms, layered and dendritic structures on their upper surfaces. These features distinguish them morphologically from yardangs observed in other planetary regions. Prominent attributes include truncated heads, aligned wings, and conical tails. The widespread distribution of these yardangs in Aeolis Planum, along with their unique structural traits, highlights their significance as analogs for comparative planetary geomorphology studies.

Conclusion

The findings of this study demonstrate that aeolian erosion is the primary force driving the formation and evolution of yardangs in both regions. Persistent, high-energy winds have sculpted elongated, linear landforms by removing loose and less resistant materials through abrasion and deflation processes. The dominant orientation of yardangs in both areas aligns with the prevailing wind direction, as evidenced by the northwest-southeast elongation of yardangs and their intervening corridors in both the Lut Desert and Aeolis Planum on Mars. However, the directional patterns of prevailing winds differ between the two regions: winds in Aeolis Planum predominantly blow from the southeast to the northwest, whereas in the Lut Desert, the dominant winds follow a northwest-southeast trajectory. This divergence in wind regimes reflects distinct climatic conditions and dynamic wind patterns across the two planetary environments.

In terms of evolutionary stages, the Lut Desert yardangs are predominantly in a mature developmental phase, characterized by elongated ridges, narrow corridors, and steep windward slopes. In contrast, the Aeolis Planum yardangs are primarily classified as "whaleback" or "hogback" types, indicative of advanced-stage erosion and geomorphological evolution. These observations suggest that the Martian yardangs in Aeolis Planum are temporally older than their terrestrial counterparts in the Lut Desert, having undergone prolonged erosional processes under Mars’ unique atmospheric and geological conditions.