The cycle of dust on Mars is a key component of current climate, is relevant in the dynamic and thermodynamic evolution of atmosphere, and is directly involved in the water cloud formation. Furthermore, dust suspended in the atmosphere is a major driver of atmospheric motions at all scales and is suspected of having had great influence on the morphological evolution of the Martian surface. The dust dispersed in the atmosphere thermally influences the behaviour of the lower atmosphere. Most of information on the nature of small particle on Mars is derived from Viking Lander data and Mars Pathfinder observations, even if the Viking orbiter IRTM instrument also was able to provide estimates of particle size distribution of Martian soil. On the other hand water is important as indicator of global climate changes on long timescale. Seasonal variations in the column abundance are due to the combined effect of exchange of H2O between atmosphere and water reservoirs (e.g. polar caps, regolith) and atmospheric transport. The Viking orbiters collected accurate information during the period 1976-1979 and much of what we know about water circulation in the Martian atmosphere derives from the observations by the Mars Atmospheric Water Detection experiments (MAWD). Despite the low absolute water content (0,03%), relative humidity can exceed 100%, leading to the formation of near surface fog and condensation clouds, thanks to low typical Mars temperatures. The typical value of 6.1 mbar (coincident with the triple point in the water phase diagram) of the surficial pressure, makes rather difficult the persistence of liquid water at the surface of Mars. This means that the water is present exclusively in a gaseous and (when the conditions are favourable) solid state. In this context, it is extremely important to study the role of the different contributions to the production of atmospheric water and to the formation of water ice clouds by the three main reservoirs, i.e. the caps, the regolith and the ice hazes. Ice hazes, in fact, provide a mechanism for scavenging water vapor in the thin Mars atmosphere and may play a key role in the seasonal cycle of water on Mars. A focused investigation, made in different regions, possibly in different seasons, and spanning several days is desirable for solving the question of linkage of water cycle with these sources. The objective of our research program is the development and production of a microbalance measurement system . Quartz crystal piezoelectric sensors are suitable for analyses that need very high sensitivity. Due to the wide working ranges (five orders of magnitude) and high sensitivity (10-6 10-11 g), microbalances can measure the mass settling in average Mars conditions during months before saturation is reached. This ensures a proper use for short and long term water vapour and dust variations monitoring. These instruments were already studied, calibrated and used for the GIADA (Grain Impact And Dust Accumulator) - Rosetta project. Long experience on microbalance performance study by dust deposition has acquired and a simulation chamber of Martian atmosphere, for water vapor deposition studies, has been prepared. It will be able to measure in situ, for the first time, directly and quantitatively, the cumulative dust mass flux and the water vapour abundance in a Martian environment. A preliminary study of this process at Mars average conditions showed that available microbalances can detect water ice condensed on their surface in few seconds, after dew or frost point is reached and similar evaluations have been made with respect to expected dust deposition rate on Mars surface, based on data from MAE experiment onboard the Sojourner rover. The measuring system will be devoted to study the dynamic of the Martian water and dust cycles. In detail, our goals are: - Study of the Martian water and dust cycles (seasonal, diurnal) and their links; - Investigation of the brines formation and evaporation mechanisms and their interaction with the regolith; - Investigation of mechanism of diurnal water release by the regolith and its weight as water atmospheric reservoir; - Study of the dust settling rates and their possible correlation with environmental conditions at the landing sites (temperature, pressure, winds); - Study of the local dust storm and devils raising mechanisms; - Investigation of the main modes of aeolian transport of grains and dust raising.We discuss the use of microbalances for the scientific applications to Martian environment studies.