Radar observations of the surface of Mercury had revealed areas with bright reflective properties in both polar regions of the planet. It was suggested that such areas contain depositions of volatile compounds, including water. In this paper, we investigated migration of water molecules to the permanently shaded areas, located in the impact crater in the polar regions of Mercury. To simulate the migration of water molecules in the exosphere of Mercury, we used the Monte Carlo method. To estimate the proportion of water molecules falling into cold traps in the polar regions of Mercury, we estimated the area of such regions. We found that the area of permanently shaded areas near the north pole of the planet reaches 23,300 km², and in the area of the south pole—45,500 km². Most of the water molecules (~ 92%) will be destroyed as a result of photolysis, and ~ 7.5% of them will be destroyed while they are on the planet's surface between hops. The fraction of water molecules that left the planet's exosphere as a result of reaching the escape velocity is only 0.3%. The fraction of water molecules trapped in permanently shaded areas in the polar regions of Mercury reaches 7.8% of the total number of particles participating in the simulation. Only 2.2% of them can be trapped in cold traps in the North Pole region and 5.6% in the South Pole region.

对水星表面的雷达观测揭示了水星两极地区具有明亮反射特性的区域。有人提出，这些区域含有挥发性化合物的沉积物，包括水。在本文中，我们研究了水分子迁移到位于水星极地撞击坑中的永久阴影区域。为了模拟水分子在水星外逸层中的迁移，我们使用了蒙特卡罗方法。为了估计水分子落入水星极地冷阱的比例，我们估计了这些区域的面积。我们发现，地球北极附近的永久阴影区域达到23,300 km ²，而在南极的区域——45,500 km ². 大多数水分子（约 92%）会因光解而被破坏，其中约 7.5% 的水分子会在跳跃之间在地球表面上被破坏。由于达到逃逸速度而离开地球外逸层的水分子比例仅为 0.3%。被困在水星极地永久阴影区域的水分子比例达到参与模拟的粒子总数的 7.8%。其中只有 2.2% 可以被困在北极地区的冷阱中，而在南极地区则为 5.6%。