Determining the launching regions of centrifugally-driven disc winds from non-ideal MHD simulations

Protostellar discs play an important role in star formation, acting as the primary mass reservoir for accretion onto young stars and regulating the extent to which angular momentum and gas is released back into stellar nurseries through the launching of powerful disc winds. In this talk, we present a novel approach to modelling the wind-launching region in protostellar disks, which enables us to map out the regions of protostellar disks where wind launching could be viable. We combine a series of 1.5D semi-analytic, steady-state, vertical disc-wind solutions into a radially extended 1+1.5D model, incorporating all three diffusion mechanisms (Ohm, Hall and ambipolar). From these models we observe that the majority of mass outflow via disc winds occurs over a radial width of a fraction of an astronomical unit, with outflow rates attenuating rapidly on either side. We also find that the mass accretion rate, midplane plasma beta, surface density profile and ionisation structure each have significant effects on both the location of the wind-launching region and the ejection/accretion ratio