Abstract
In this paper, an initiative Martian dust fluid simulating research based on the energy dissipation method was developed to simulate the deposition process of Martian dust fluid which was caused by surface adhesion between particles and Martian rovers. Firstly, an energy dissipation model of particles based on the Discrete Element Method (DEM) was established because of the characteristics of Martian dust particles such as tiny size and viscoelasticity. This model is based on the existing DMT model to analyze the collision deposition of dust fluid particles, including particle-spacecraft collision and particle-particle collision. Secondly, this paper analyzed the characteristics of particles after their first collision, then, established the stochastic model of critical wind speed for the particle deposition process. Finally, a series of simulations of the Martian dust fluid particle deposition process were done based on DEM-CFD. The results verified the accuracy of the energy dissipation model and the stochastic model, which could also verify the feasibility and effectiveness of the computing method of Martian dust fluid based on the DEM-CFD technology.
Highlights
A global dust storm (GDS) occurred in Mars year (MY) 34 (2018)
An initiative Martian dust fluid simulating research based on the energy dissipation method was developed to simulate the deposition process of Martian dust fluid which was caused by surface adhesion between particles and Martian rovers
The energy dissipation of collision is defined as the combined effect of adhesion energy loss and damping energy loss, and the contact status of Martian dust particles is analyzed based on the DMT contact model [33]
Summary
A global dust storm (GDS) occurred in Mars year (MY) 34 (2018). According to the observation from the MSL Curiosity rover, the daily maximum UV radiation in the Gale Crater decreased by 90% from sols 2075 (opacity~1) to sols 2085 (opacity~8.5) [1, 2]. Every few Mars years, regional dust storms grow and merge to become a global dust storm (GDS). The timeline includes all major planetencircling and regional dust storms, which were observed by Mars orbiters, by Mars landers or by telescopes from the Earth, from 1971 to 2013 (the MY9 to the MY31) [3–7]. According to limited GDS samples, a GDS occurred every three Mars years on average
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