论文标题
火星灰尘环的配置：粒子轨迹直接整合的形状，密度和尺寸分布
Configuration of the Martian dust rings: Shapes, densities and size-distributions from direct integrations of particle trajectories
论文作者
论文摘要
自1970年代初以来，预计脆弱的灰尘环是由火星卫星phobos和Deimos弹出的谷物形成的。在本文中，我们对源自Phobos和Deimos的大量灰尘颗粒进行直接数值整合。在发明的模拟中，包括作用于灰尘的最相关的力包括：球形谐波高达5度和第五阶的火星重力，太阳，phobos和Deimos的引力扰动，太阳辐射压力以及poynting-Robertson drag。为了获得环构型，在弹出的指定初始质量分布上平均各种晶粒尺寸的模拟结果平均。我们发现，对于小于大约2微米的Phobos环晶粒而言是主要的。而Deimos环在约5-20微米的尺寸范围内以灰尘为主。通过模拟来量化环的不对称，数量密度和几何光学深度。将结果与哈勃观测得出的光学深度的上限进行了比较。我们将与以前的工作进行比较，并讨论模型的不确定性。
It is expected since the early 1970s that tenuous dust rings are formed by grains ejected from the Martian moons Phobos and Deimos by impacts of hypervelocity interplanetary projectiles. In this paper, we perform direct numerical integrations of a large number of dust particles originating from Phobos and Deimos. In the numerical simulations, the most relevant forces acting on dust are included: Martian gravity with spherical harmonics up to 5th degree and 5th order, gravitational perturbations from the Sun, Phobos, and Deimos, solar radiation pressure, as well as the Poynting-Robertson drag. In order to obtain the ring configuration, simulation results of various grain sizes ranging from submicron to 100 microns are averaged over a specified initial mass distribution of ejecta. We find that for the Phobos ring grains smaller than about 2 microns are dominant; while the Deimos ring is dominated by dust in the size range of about 5-20 microns. The asymmetries, number densities and geometrical optical depths of the rings are quantified from simulations. The results are compared with the upper limits of the optical depth inferred from Hubble observations. We compare to previous work and discuss the uncertainties of the models.
