  Active regions are thought to be one contributor to the slow solar wind.
Upflows in EUV coronal spectral lines are routinely osberved at their
boundaries, and provide the most direct way for upflowing material to escape
into the heliosphere. The mechanisms that form and drive these upflows,
however, remain to be fully characterised. It is unclear how quickly they form,
or how long they exist during their lifetimes. They could be initiated low in
the atmosphere during magnetic flux emergence, or as a response to processes
occuring high in the corona when the active region is fully developed. On 2019,
March 31, a simple bipolar active region (AR 12737) emerged and upflows
developed on each side. We used observations from Hinode, SDO, IRIS, and Parker
Solar Probe (PSP) to investigate the formation and development of the upflows
from the eastern side. We used the spectroscopic data to detect the upflow, and
then used the imaging data to try to trace its signature back to earlier in the
active region emergence phase. We find that the upflow forms quickly, low down
in the atmosphere, and that its initiation appears associated with a small
field-opening eruption and the onset of a radio noise storm detected by PSP. We
also confirmed that the upflows existed for the vast majority of the time the
active region was observed. These results suggest that the contribution to the
solar wind occurs even when the region is small, and continues for most of its
lifetime.
