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Stars form in highly-magnetised, supersonic turbulent molecular clouds. Manyof the tools and models that we use to carry out star formation studies relyupon the assumption of cloud isotropy. However, structures like high-densityfilaments in the presence of magnetic fields, and magnetosonic striationsintroduce anisotropies into the cloud. In this study we use the two-dimensional(2D) power spectrum to perform a systematic analysis of the anisotropies in thecolumn density for a range of Alfv\'en Mach numbers ($\mathcal{M}_A=0.1$--$10$)and turbulent Mach numbers ($\mathcal{M}=2$--$20$), with 20 high-resolution,three-dimensional (3D) turbulent magnetohydrodynamic simulations. We find thatfor cases with a strong magnetic guide field, corresponding to$\mathcal{M}_A<1$, and $\mathcal{M}\lesssim 4$, the anisotropy in the columndensity is dominated by thin striations aligned with the magnetic field, whilefor $\mathcal{M}\gtrsim 4$ the anisotropy is significantly changed byhigh-density filaments that form perpendicular to the magnetic guide field.Indeed, the strength of the magnetic field controls the degree of anisotropyand whether or not any anisotropy is present, but it is the turbulent motionscontrolled by $\mathcal{M}$ that determine which kind of anisotropy dominatesthe morphology of a cloud.

Filaments and striations: anisotropies in observed, supersonic, highly-magnetised turbulent clouds