We present observations of O VI 1032 A line profiles obtained with the SUMER instrument on SOHO extending from the solar disk to 1.5 R_/odot above the limb in the north polar coronal hole. Variations of the intensity and line width in the polar plume and inter-plume regions are investigated. We find an anti-correlation between the intensity and the line width in the plume and inter-plume regions with detailed plume structures been seen out to 1.5 R_/odot. Possible implications regarding the magnetic topologies of these two regions and related heating mechanisms are discussed. The O VI line width measurements are combined with UVCS output to provide an overview of its variations with height extending up to 3.5 R_/odot. We find a linear increase of the line width from 1 to 1.2 R_/odot, then a plateau followed by a sharp increase around 1.5 R_/odot.