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We present a set of numerical experiments designed to systematicallyinvestigate how turbulence and magnetic fields influence the morphology,energetics, and dynamics of filaments produced in wind-cloud interactions. Wecover 3D magnetohydrodynamic systems of supersonic winds impacting clouds withturbulent density, velocity, and magnetic fields. We find that log-normaldensity distributions aid shock propagation through clouds, increasing theirvelocity dispersion and producing filaments with expanded cross sections andhighly-magnetised knots and sub-filaments. In self-consistently turbulentscenarios the ratio of filament to initial cloud magnetic energy densities is~1. The effect of Gaussian velocity fields is bound to the turbulence Machnumber: Supersonic velocities trigger a rapid cloud expansion; subsonicvelocities only have a minor impact. The role of turbulent magnetic fieldsdepends on their tension and is similar to the effect of radiative losses: thestronger the magnetic field or the softer the gas equation of state, thegreater the magnetic shielding at wind-filament interfaces and the suppressionof Kelvin-Helmholtz instabilities. Overall, we show that including turbulenceand magnetic fields is crucial to understanding cold gas entrainment inmulti-phase winds. While cloud porosity and supersonic turbulence enhance theacceleration of clouds, magnetic shielding protects them from ablation andcauses Rayleigh-Taylor-driven sub-filamentation. Wind-swept clouds in turbulentmodels reach distances ~15-20 times their core radius and acquire bulk speeds~0.3-0.4 of the wind speed in one cloud-crushing time, which are three timeslarger than in non-turbulent models. In all simulations the ratio of turbulentmagnetic to kinetic energy densities asymptotes at ~0.1-0.4, and convergence ofall relevant dynamical properties requires at least 64 cells per cloud radius.

Filament formation in wind-cloud interactions. II. Clouds with turbulent density, velocity, and magnetic fields