  Global and mesoscale models represent the background (slowly varying) winds
on Mars, but short timescale wind variability is not explicitly represented.
The local wind erosion and dust deposition model can be useful for more
accurate local wind friction, wind friction threshold, horizontal sand flux and
vertical 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 of
threshold wind friction estimation and takes into account the influence of
atmospheric electric fields on sand and dust elevation processes. The model
parameterized for the Earth was tested on data acquired in Morocco field
campaign 2013-2014 (Esposito et al.,) \cite{Esposito}, \cite{Esposito2}. Wind
friction, wind friction threshold, horizontal sand flux and vertical dust flux
were simulated by using the following inputs measured in the field: wind speed,
wind direction, air temperature, air pressure, air humidity, solar irradiation
and surface roughness length. The same inputs are supposed to be measured by
DREAMs equipment on Mars (except for the surface roughness length which can be
estimated for Mars according the method of Hebrard \cite{Hebrard}). Simulated
and experimental values have shown a good agreement. The model was adapted to
Martian conditions and applied to the data of Viking lander. The local wind
erosion and dust deposition model parameterized for Mars may serve 1) to
analyze local lander/rovers data, 2) a source of local parameters/inputs (like
threshold wind friction velocity, sand and dust fluxes) for the MGCM (Mars
Global Circulation Model).
