导致HD 61005周围尘埃形状形态的星际风特性
Properties of interstellar wind leading to shape morphology of the dust surrounding HD 61005
摘要：
在散射光中观察到从HD 61005周围的碎片环喷出的尘埃颗粒形成的结构。这里的主要目的是限制星际风参数，导致形状形态在HD 61005附近使用目前可用的观测数据的碎片环。求解了2 $\times$ 10 $^5$尘埃粒子在电磁辐射、恒星风和星际风作用下从碎片环中喷出的运动方程。一个二维（2D）网格被放置在一个给定的方向上的灰尘颗粒上散射的光的积累，以确定形状形态。考虑了星际风和恒星风的相互作用。确定了创造所观察到的形态的星际风的未知属性组。找到了星际风中气体组分数密度与其相对速度的关系，研究了与不同温度的星际云相互作用所引起的形状形态的变化。当星际风速度从碎片环轴倾斜时，星际风的性质与视线和星际风速度之间的角度之间存在简单的关系。受恒星辐射影响最大的尘埃粒子在观测结构的边界上移动。在HD 61005观测到的结构可以解释为尘埃粒子在星际风的作用下移动的结果。星际风所需的数密度或速度比进入太阳系的星际风要高得多。
英文摘要：
A structure formed by dust particles ejected from the debris ring around HD 61005 is observed in the scattered light. The main aim here is to constrain interstellar wind parameters that lead to shape morphology in the vicinity of HD 61005 using currently available observational data for the debris ring. Equation of motion of 2 $\times$ 10$^5$ dust particles ejected from the debris ring under the action of the electromagnetic radiation, stellar wind, and interstellar wind is solved. A two-dimensional (2D) grid is placed in a given direction for accumulation of the light scattered on the dust particles in order to determine the shape morphology. The interaction of the interstellar wind and the stellar wind is considered. Groups of unknown properties of the interstellar wind that create the observed morphology are determined. A relation between number densities of gas components in the interstellar wind and its relative velocity is found. Variations of the shape morphology caused by the interaction with the interstellar clouds of various temperatures are studied. When the interstellar wind velocity is tilted from debris ring axis a simple relation between the properties of the interstellar wind and an angle between the line of sight and the interstellar wind velocity exists. Dust particles that are most significantly influenced by stellar radiation move on the boundary of observed structure. Observed structure at HD 61005 can be explained as a result of dust particles moving under the action of the interstellar wind. Required number densities or velocities of the interstellar wind are much higher than that of the interstellar wind entering the Solar system.
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