The global structure of astrospheres: effect of Knudsen number

TL;DR

This paper investigates how the global structure of astrospheres depends on the Knudsen number, using a kinetic model to analyze neutral-plasma interactions across a wide range of conditions, revealing limitations of single-fluid models.

Contribution

It introduces a kinetic-gas dynamics model to study astrosphere structures over various Knudsen numbers, highlighting the formation of a heated plasma layer and the inadequacy of single-fluid approaches.

Findings

A heated plasma layer forms in large astrospheres with high Knudsen numbers.

Single-fluid models cannot accurately describe the flow structure near the astropause.

Atoms significantly influence bow shock properties at near-heliospheric conditions.

Abstract

The interaction between stellar winds and the partially ionized local interstellar medium (LISM) is quite common in astrophysics. However, the main difficulty in describing the neutral components lies in the fact that the mean free path of an interstellar atom, l, can be comparable to the characteristic size of an astrosphere, L (i.e., the Knudsen number, which is equal to l/L, is approximately equal to 1, as in the case of the heliosphere). In such cases, a single-fluid approximation becomes invalid, and a kinetic description must be used for the neutral component. In this study, we consider a general astrosphere and use a kinetic-gas dynamics model to investigate how the global structure of the astrosphere depends on the Knudsen number. We present numerical results covering an extremely wide range of Knudsen numbers (from 0.0001 to 100). Additionally, we explore the applicability of single-fluid approaches for modeling astrospheres of various sizes. We have excluded the influence of interstellar and stellar magnetic fields in our model to make parametric study of the kinetic effects feasible. The main conclusion of this work is that, for large astrospheres (with a distance to the bow shock greater than 600 AU) a heated rarefied plasma layer forms in the outer shock layer near the astropause. The formation of this layer is linked to localized heating of the plasma by atoms (specifically, ENAs) that undergo charge exchange again behind the astropause. This process significantly alters the flow structure in the outer shock layer and the location of the bow shock, and it cannot be described by a single-fluid model. Additionally, this paper discusses how atoms weaken the bow shocks at near-heliospheric conditions.