Hydrodynamical models of clumping beyond 50 stellar radii

TL;DR

This paper develops 1D time-dependent hydrodynamical models of stellar wind clumping caused by line-deshadowing instability, demonstrating that clumping persists beyond 50 stellar radii into the radio continuum formation region.

Contribution

It introduces an efficient moving-box technique to simulate wind clumping out to over 1000 stellar radii, extending previous models.

Findings

Clumping persists beyond 50 stellar radii.

Wind remains clumped into the radio continuum formation region.

The moving-box technique enables long-distance wind simulations.

Abstract

We present one-dimensional, time-dependent models of the clumps generated by the line-deshadowing instability. In order to follow the clumps out to distances of more than 1000 stellar radii, we use an efficient moving-box technique. We show that, within the approximations, the wind can remain clumped well into the formation region of the radio continuum.