From Doppler velocity maps of active regions constructed from spectra obtained by the Extreme-ultraviolet Imaging Spectrometer ( EIS ) on the Hinode spacecraft we observe large areas of outflow ( 20-50 km s ^ { -1 } ) that can persist for at least a day .
These outflows occur in areas of active regions that are faint in coronal spectral lines formed at typical quiet Sun and active region temperatures .
The outflows are positively correlated with non-thermal velocities in coronal plasmas .
The bulk mass motions and non-thermal velocities are derived from spectral line centroids and line widths , mostly from a strong line of Fe xii at 195.12 Å .
The electron temperature of the outflow regions estimated from an Fe xiii to Fe xii line intensity ratio is about 1.2 - 1.4 \times 10 ^ { 6 } K. The electron density of the outflow regions derived from a density sensitive intensity ratio of Fe xii lines is rather low for an active region .
Most regions average around 7 \times 10 ^ { 8 } cm ^ { -3 } , but there are variations on pixel spatial scales of about a factor of 4 .
We discuss results in detail for two active regions observed by EIS .
Images of active regions in line intensity , line width , and line centroid are obtained by rastering the regions .
We also discuss data from the active regions obtained from other orbiting spacecraft that support the conclusions obtained from analysis of the EIS spectra .
The locations of the flows in the active regions with respect to the longitudinal photospheric magnetic fields suggest that these regions might be tracers of long loops and/or open magnetic fields that extend into the heliosphere , and thus the flows could possibly contribute significantly to the solar wind .