Properties of interstellar wind leading to shape morphology of the dust surrounding HD 61005

TL;DR

This study models how interstellar wind parameters influence the dust morphology around HD 61005, revealing that higher wind densities and velocities shape the observed dust structures, with implications for understanding interstellar interactions.

Contribution

The paper introduces a detailed model of dust particle dynamics around HD 61005 considering interstellar, stellar, and electromagnetic forces, linking wind properties to observed dust morphology.

Findings

Interstellar wind parameters significantly affect dust structure shape.

A relation between gas densities, velocities, and morphology angle is established.

Dust particles influenced by stellar radiation define the observed boundary.

Abstract

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.