The origin of slow Alfv\'enic solar wind at solar minimum

Although the origins of slow solar wind are unclear, there is increasing evidence that at least some of it is released in a steady state on over-expanded coronal hole magnetic field lines. This type of slow wind has similar properties to the fast solar wind, including a high degree of Alfvenicity. In this study a combination of proton, alpha particle, and electron measurements are used to investigate the kinetic properties of a single interval of slow Alfvenic wind at 0.35 AU. It is shown that this slow Alfvenic interval is characterised by high alpha particle abundances, pronounced alpha-proton differential streaming, strong proton beams, and large alpha to proton temperature ratios. These are all features observed consistently in the fast solar wind, adding evidence that at least some Alfvenic slow solar wind also originates in coronal holes. Observed differences between speed, mass flux, and electron temperature between slow Alfvenic and fast winds are explained by differing magnetic field geometry in the lower corona.