  The higher charge states found in slow ($<$400km s$^{-1}$) solar wind streams
compared to fast streams have supported the hypothesis that the slow wind
originates in closed coronal loops, and released intermittently through
reconnection. Here we examine whether a highly ionized slow wind can also form
along steady and open magnetic field lines. We model the steady-state solar
atmosphere using AWSoM, a global magnetohydrodynamic model driven by Alfv{\'e}n
waves, and apply an ionization code to calculate the charge state evolution
along modeled open field lines. This constitutes the first charge states
calculation covering all latitudes in a realistic magnetic field. The ratios
$O^{+7}/O^{+6}$ and $C^{+6}/C^{+5}$ are compared to in-situ Ulysses
observations, and are found to be higher in the slow wind, as observed;
however, they are under-predicted in both wind types. The modeled ion fractions
of S, Si, and Fe are used to calculate line-of-sight intensities, which are
compared to EIS observations above a coronal hole. The agreement is partial,
and suggests that all ionization rates are under-predicted. Assuming the
presence of suprathermal electrons improved the agreement with both EIS and
Ulysses observations; importantly, the trend of higher ionization in the slow
wind was maintained. The results suggest there can be a sub-class of slow wind
that is steady and highly ionized. Further analysis shows it originates from
coronal hole boundaries (CHB), where the modeled electron density and
temperature are higher than inside the hole, leading to faster ionization. This
property of CHBs is global, and observationally supported by EUV tomography.
