  We investigate the evolution of a well-observed, long-lived, low-latitude
coronal hole (CH) over 10 solar rotations in the year 2012. By combining EUV
imagery from STEREO-A/B and SDO we are able to track and study the entire
evolution of the CH having a continuous 360$\deg$ coverage of the Sun. The
remote sensing data are investigated together with in-situ solar wind plasma
and magnetic field measurements from STEREO-A/B, ACE and WIND. From this we
obtain how different evolutionary states of the CH as observed in the solar
atmosphere (changes in EUV intensity and area) affect the properties of the
associated high-speed stream measured at $1$AU. Most distinctly pronounced for
the CH area, three development phases are derived: a) growing, b) maximum, and
c) decaying phase. During these phases the CH area a) increases over a duration
of around three months from about $1 \cdot 10^{10} \mathrm{km}^{2}$ to $6 \cdot
10^{10} \mathrm{km}^{2}$, b) keeps a rather constant area for about one month
of $> 9 \cdot 10^{10} \mathrm{km}^{2}$, and c) finally decreases in the
following three months below $1 \cdot 10^{10} \mathrm{km}^{2}$ until the CH
cannot be identified anymore. The three phases manifest themselves also in the
EUV intensity and in in-situ measured solar wind proton bulk velocity.
Interestingly, the three phases are related to a different range in solar wind
speed variations and we find for the growing phase a range of
$460-600$~km~s$^{-1}$, for the maximum phase $600-720$~km~s$^{-1}$, and for the
decaying phase a more irregular behavior connected to slow and fast solar wind
speed of $350-550$~km~s$^{-1}$.
