Ionisation in turbulent magnetic molecular clouds

Abstract

Previous studies show that the physical structures and kinematics of a region depend significantly on the ionisation fraction. In this paper, we extend our previous studies of the effect of ionisation fractions on star formation to clouds that include both non-ideal magnetohydrodynamics and turbulence. We aim to quantify the importance of a treatment of the ionisation fraction in turbulent magnetised media and investigate the effect of turbulence on shaping the clouds and filaments before star formation sets in. In particular, we investigate how the structure, mass and width of filamentary structures depend on the amount of turbulence in ionised media and the initial mass-to-flux ratio. We compare the resulting density and mass-to-flux ratio structures both qualitatively and quantitatively via filament and core masses and filament fitting techniques (Gaussian and Plummer profiles.) We find that even with almost no turbulence, filamentary structure still exists. Comparison of simulations show that for turbulent Mach numbers above 2, there is little structural difference between the Step-Like (SL) and Cosmic Ray only (CR-only) ionisation models, while below this threshold the ionisation structure significantly affects the formation of filaments. Analysis of the mass within cores and filaments show decrease in mass as the degree of turbulence increases. Finally, observed filaments within the Taurus L1495/B213 complex are best reproduced by models with supercritical mass-to-flux ratios and/or at least mildly supersonic turbulence, however, our models show that sterile fibres observed within Taurus may occur in highly ionised, subcritical environments. Based on this, we suggest that regions with fertile fibres likely indicate a trans- or supercritical mass-to-flux ratio within the region while sterile fibres are likely subcritical and transient.