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 \arcdeg 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 can not 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 } .