arXiv2012
(abridged) The nature of early Class 0/I protostellar discs is not clearly understood. Early protostellar discs are needed to drive molecular outflows and jets observed in star forming regions, but there has been some debate to how they form. From a theoretical perspective, the consequences of disc and outflow generation are crucial to understanding the very nature of how stars are assembled. We have performed 3D ideal magnetohydrodynamic (MHD) simulations of collapsing Bonnor-Ebert spheres, employing sink particles with a radius of 3.2 AU alongside an AMR grid and using a cooling function to model radiative cooling of the gas. This has allowed us to explore 2-8x10^4 yr further into the evolution of an early Class 0 disc-outflow system than previous simulations. Our outflow is precessing, kinked, turbulent, contains internal shocks and has a scale of 0.1 pc end-to-end. We form a rotationally dominated disc with a radius of 100 AU embedded inside a transient, unstable, flattened, rotating core extending out to 2000 AU. The larger flattened structure launches a low speed wind (v_r < 1.5 km/s) dominated by B_phi, while the inner disc launches a centrifugally driven jet dominated by B_p with speeds up to 20$ km/s. From the inner disk, the value of dM/dt_out/dM/dt_in ~ 0.1, wheras in the outer core dM/dt_out/dM/dt_in ~ 1.0. The inner disc becomes unstable to a warping instability due to the magnetic structure of the outflow and warps to 30 deg with respect to the z-axis by the end of the simulation. The envelope is cleared out and is less massive than the disc. We measure star formation efficiencies of eta_core=0.63 (and growing), higher than theoretical predictions. This indicates that outflows are not as efficient at expelling envelope mass as some current models estimate. We discuss the relevance of our disc misalignment concerning the formation of mis-aligned hot Jupiters.