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Previous studies show that the physical structures and kinematics of a regiondepend significantly on the ionisation fraction. In this paper, we extend ourprevious studies of the effect of ionisation fractions on star formation toclouds that include both non-ideal magnetohydrodynamics and turbulence. We aimto quantify the importance of a treatment of the ionisation fraction inturbulent magnetised media and investigate the effect of turbulence on shapingthe clouds and filaments before star formation sets in. In particular, weinvestigate how the structure, mass and width of filamentary structures dependon the amount of turbulence in ionised media and the initial mass-to-fluxratio. We compare the resulting density and mass-to-flux ratio structures bothqualitatively and quantitatively via filament and core masses and filamentfitting techniques (Gaussian and Plummer profiles.) We find that even withalmost no turbulence, filamentary structure still exists. Comparison ofsimulations show that for turbulent Mach numbers above 2, there is littlestructural difference between the Step-Like (SL) and Cosmic Ray only (CR-only)ionisation models, while below this threshold the ionisation structuresignificantly affects the formation of filaments. Analysis of the mass withincores and filaments show decrease in mass as the degree of turbulenceincreases. Finally, observed filaments within the Taurus L1495/B213 complex arebest reproduced by models with supercritical mass-to-flux ratios and/or atleast mildly supersonic turbulence, however, our models show that sterilefibres observed within Taurus may occur in highly ionised, subcriticalenvironments. Based on this, we suggest that regions with fertile fibres likelyindicate a trans- or supercritical mass-to-flux ratio within the region whilesterile fibres are likely subcritical and transient.

Ionisation in Turbulent Magnetic Molecular Clouds I. Effect on Density and Mass-to-Flux Ratio Structures