Charging of Interstellar Dust Grains Near the Heliopause

TL;DR

This paper investigates how interstellar dust grain aggregates acquire charge near the heliopause, affecting their deflection in magnetic fields, with implications for interpreting in-situ measurements and matching observational data.

Contribution

It introduces a new method to estimate aggregate charge based on structural characteristics, considering plasma charging and secondary electron emission effects.

Findings

Aggregates have higher charge-to-mass ratios than spheres.

Secondary electron emission significantly affects nano-sized aggregates.

Derived mass distribution aligns with Ulysses observational data.

Abstract

The deflection of interstellar dust grains in the magnetic field near the heliopause has been investigated based on the assumption that interstellar grains are homogeneous spheres. However, remote observations have shown that interstellar grains are more likely to be composites of a large number of subunits. This has profound significance when interpreting data obtained through in-situ measurements, for the deflection of interstellar grains depends on their charge-to-mass ratio, and aggregates acquire different surface charges from spheres due to their complex structure. In this paper, the charging of aggregates near the heliopause is examined including both plasma charging and secondary electron emission. The results show that aggregates generally have a higher charge-to-mass ratio than spheres, and the small particle effect from secondary electron emission is evident for aggregates consisting of nano-sized particles. A new approach to estimate the aggregate charge with the aid of its structural characteristics is presented. The charge-to-mass ratio is used to derive the mass distribution of interstellar dust near the heliopause, and the result shows an overall agreement with Ulysses data.