Filament formation in wind-cloud interactions. I. Spherical clouds in uniform magnetic fields

TL;DR

This study uses advanced numerical simulations to explore how supersonic winds interacting with dense spherical clouds in magnetic fields produce filamentary structures, revealing their formation mechanisms, properties, and effects of magnetic field variations.

Contribution

It provides detailed insights into filament formation in wind-cloud interactions, including the influence of magnetic field strength and orientation, with improved simulation resolution and density contrasts.

Findings

Filaments have aspect ratios >12 and magnetic amplification ~100.

Magnetic fields influence filament turbulence and structure.

Cloud material forms tails and flux ropes, surviving cloud break-up.

Abstract

Filamentary structures are ubiquitous in the interstellar medium, yet their formation, internal structure, and longevity have not been studied in detail. We report the results from a comprehensive numerical study that investigates the characteristics, formation, and evolution of filaments arising from magnetohydrodynamic interactions between supersonic winds and dense clouds. Here we improve on previous simulations by utilising sharper density contrasts and higher numerical resolutions. By following multiple density tracers, we find that material in the envelopes of the clouds is removed and deposited downstream to form filamentary tails, while the cores of the clouds serve as footpoints and late-stage outer layers of these tails. Aspect ratios >12, subsonic velocity dispersions ~0.1-0.3 of the wind sound speed, and magnetic field amplifications ~100 are found to be characteristic of these filaments. We also report the effects of different magnetic field strengths and orientations. The magnetic field strength regulates vorticity production: sinuous filamentary towers arise in non-magnetic environments, while strong magnetic fields inhibit small-scale perturbations at boundary layers making tails less turbulent. Magnetic field components aligned with the direction of the flow favour the formation of pressure-confined flux ropes inside the tails, whilst transverse components tend to form current sheets. Softening the equation of state to nearly isothermal leads to suppression of dynamical instabilities and further collimation of the tail. Towards the final stages of the evolution, we find that small cloudlets and distorted filaments survive the break-up of the clouds and become entrained in the winds, reaching velocities ~0.1 of the wind speed.