研究了尘埃粒子在快速星际气体流作用下的轨道演化。长期的时间导数开普勒轨道要素和径向，横向和正常的组成部分的气体流速度矢量在近心点的粒子的轨道推导。在粒子轨道的近心点处的半长轴、偏心率以及气流速度矢量的径向、横向和法向分量的长期时间导数构成方程组，该方程组确定粒子轨道相对于气流速度矢量在空间中的演化。这个微分方程组可以很容易地用解析法求解。从该系统的解决方案，我们发现的开普勒轨道元素的演化的特殊情况下，当轨道元素确定相对于一个平面垂直于气流速度矢量。给出了将这种特殊情况下确定的开普勒轨道根数变换为相对于任意定向平面确定的轨道根数的方法。尘埃粒子的轨道根数以恒定的振荡周期周期性地变化或保持恒定。讨论了平面、垂直和静止解。本文还讨论了该解在太阳系中的适用性。我们考虑半径从1到10微米的冰粒子。所提出的解决方案是有效的，这些粒子的轨道与半长轴从200至3000 AU和偏心率小于0.8，大约。这些轨道的振荡周期大约在10^5到2 x 10^6年之间。
英文摘要：
The orbital evolution of a dust particle under the action of a fast interstellar gas flow is investigated. The secular time derivatives of Keplerian orbital elements and the radial, transversal, and normal components of the gas flow velocity vector at the pericentre of the particle's orbit are derived. The secular time derivatives of the semi-major axis, eccentricity, and of the radial, transversal, and normal components of the gas flow velocity vector at the pericentre of the particle's orbit constitute a system of equations that determines the evolution of the particle's orbit in space with respect to the gas flow velocity vector. This system of differential equations can be easily solved analytically. From the solution of the system we found the evolution of the Keplerian orbital elements in the special case when the orbital elements are determined with respect to a plane perpendicular to the gas flow velocity vector. Transformation of the Keplerian orbital elements determined for this special case into orbital elements determined with respect to an arbitrary oriented plane is presented. The orbital elements of the dust particle change periodically with a constant oscillation period or remain constant. Planar, perpendicular and stationary solutions are discussed.
The applicability of this solution in the Solar system is also investigated. We consider icy particles with radii from 1 to 10 micrometers. The presented solution is valid for these particles in orbits with semi-major axes from 200 to 3000 AU and eccentricities smaller than 0.8, approximately. The oscillation periods for these orbits range from 10^5 to 2 x 10^6 years, approximately.
High Radiation Pressure on Interstellar Dust Computed by Light-Scattering Simulation on Fluffy Agglomerates of Magnesium-silicate Grains with Metallic-iron Inclusions
Automatic detection of impact craters on Al foils from the Stardust interstellar dust collector using convolutional neural networks
Space Sciences Laboratory, University of California at Berkeley（加州大学伯克利分校空间科学实验室）；Centre for Astrophysics and Planetary Science, University of Kent（肯特大学天体物理与行星科学中心）；Washington University（华盛顿大学）
