Aeolian sand dunes are observed across the Martian surface. The arrival of HiRISE camera on Mars Reconnaissance Orbiter at in 2006 enabled detection modern-day movement and ripples from orbit for first time. Since 2006, collected a long timeseries repeat imagery few dune fields. We analyze this two these fields, using COSI-Corr image registration correlation, to study dynamics meter-scale Nili ...

There are several hotspots of dust production in the central Sahara, Bodélé Depression (BD) northern Chad is considered largest source aerosol worldwide, with fastest Barchan dunes that migrate southwesterly. Less known about complex patterns dune movement BD, especially on a short time scale. Time-series inversion optical image cross-correlation (TSI-OICC) proved to be valuable method for moni...

Wind regime and sand grain size are two of the factors that determine the morphology and dynamics of sand dunes in desert areas. Regarding the importance of wind effects on sand dunes especially in Iran, in this study, Khartooran Erg was analyzed to determine wind direction and to detect sand source sites. Khartooran Erg is located on eastern north of Iran and lies in Khorasan Razavi and Semnan...

Introduction: Mars is host to a wide range of aeolian forms such as dunes, ripples, dust devils, dust storms, yardangs, and ventifacts. Large dune fields characterized by low albedos and large duneform sizes have been observed and occur mainly around the north polar cap and in the southern mid-latitudes. However, another morphologically and dimensionally distinct population of aeolian bedforms ...

Relations of landform types to wind regimes, bedrock composition, sediment supply, and topography are shown by field studies and satellite photographs of the Western Desert of Egypt. This desert, which lies at the core of the largest hyperarid region on earth, provides analogs of Martian wind-formed features. These include sand dunes, alternating light and dark streaks, knob 'shadows,' and yard...

Introduction: Chasma Boreale, a large reentrant in the martian North Pole, is distinct from other polar troughs by its large size and counterclockwise orientation [5]. The ~ 1300 m deep chasma extends for ~ 500 km from its proposed origin at 85° N, 2o E and is on average ~ 60 km wide. The head of the feature is marked by two major steep, arcuate scarps. Extending from the mouth of Chasma Boreal...