  We study the properties of 115 coronal holes in the time-range from 2010/08
to 2017/03, the peak velocities of the corresponding high-speed streams as
measured in the ecliptic at 1 AU, and the corresponding changes of the Kp index
as marker of their geo-effectiveness. We find that the peak velocities of
high-speed streams depend strongly on both the ar- eas and the co-latitudes of
their solar source coronal holes with regard to the heliospheric latitude of
the satellites. Therefore, the co-latitude of their source coronal hole is an
im- portant parameter for the prediction of the high-speed stream properties
near the Earth. We derive the largest solar wind peak velocities normalized to
the coronal hole areas for coronal holes located near the solar equator, and
that they linearly decrease with increas- ing latitudes of the coronal holes.
For coronal holes located at latitudes & 60{\deg}, they turn statistically to
zero, indicating that the associated high-speed streams have a high chance to
miss the Earth. Similar, the Kp index per coronal hole area is highest for the
coronal holes located near the solar equator and strongly decreases with
increasing latitudes of the coronal holes. We interpret these results as an
effect of the three-dimensional propaga- tion of high-speed streams in the
heliosphere, i.e., high-speed streams arising from coro- nal holes near the
solar equator propagate in direction towards and directly hit the Earth,
whereas solar wind streams arising from coronal holes at higher solar latitudes
only graze or even miss the Earth.
