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Global and mesoscale models represent the background (slowly varying) windson Mars, but short timescale wind variability is not explicitly represented.The local wind erosion and dust deposition model can be useful for moreaccurate local wind friction, wind friction threshold, horizontal sand flux andvertical dust flux modeling on Mars. Such a model based on the model of Zender\cite{Zender} is proposed in this article. It includes different methods ofthreshold wind friction estimation and takes into account the influence ofatmospheric electric fields on sand and dust elevation processes. The modelparameterized for the Earth was tested on data acquired in Morocco fieldcampaign 2013-2014 (Esposito et al.,) \cite{Esposito}, \cite{Esposito2}. Windfriction, wind friction threshold, horizontal sand flux and vertical dust fluxwere simulated by using the following inputs measured in the field: wind speed,wind direction, air temperature, air pressure, air humidity, solar irradiationand surface roughness length. The same inputs are supposed to be measured byDREAMs equipment on Mars (except for the surface roughness length which can beestimated for Mars according the method of Hebrard \cite{Hebrard}). Simulatedand experimental values have shown a good agreement. The model was adapted toMartian conditions and applied to the data of Viking lander. The local winderosion and dust deposition model parameterized for Mars may serve 1) toanalyze local lander/rovers data, 2) a source of local parameters/inputs (likethreshold wind friction velocity, sand and dust fluxes) for the MGCM (MarsGlobal Circulation Model).

Testing a new model of local wind erosion and dust deposition on field campaign data in Morocco. Adaptation of the model for Mars