Snapshot of a magnetohydrodynamic disk wind traced by water maser observations

The formation of astrophysical objects different nature, from black holes to gaseous giant planets, involves a disk–jet system, where the disk drives mass accretion onto central compact object and jet is fast collimated ejection along rotation axis. Magnetohydrodynamic winds can provide link between ejection, which essential ensure that excess angular momentum removed proceed. However, until now, we have been lacking direct observational proof winds. Here present view velocity field wind around forming massive star. Achieving very high spatial resolution about 0.05 au, our water maser observations trace velocities individual streamlines emerging orbiting We find that, at low elevation above midplane, flow co-rotates with its launch point in disk, agreement magneto-centrifugal acceleration. Beyond co-rotation point, rises spiralling axis helical magnetic field. performed (resistive-radiative-gravito-)magnetohydrodynamic simulations star record development magneto-centrifugally launched presenting many properties observations. observation has achieved high-spatial-resolution (0.05 au) masers.