Abstract
Comparative analysis of solar wind speed variations measured by the ACE spacecraft at the L1 point and the extreme ultraviolet emission in the Fe IX-X, Fe XII, and Fe XV spectral lines from coronal holes on the SOHO/EIT observation permit us to identify areas of coronal hole that probably generate high-speed solar wind components in the lower corona. At the lower corona the emission of these areas do not coincide with details of the chromospheric network, coronal bright points, streamers which traditionally identified as sources of plasma outflow observed afterwards near the Earth as solar wind. We suppose that small-scale photospheric and chromospheric magnetic field at the coronal levels forms large structures with lines of emission/absorption, and high speed solar wind streams are generated in these large structures. The characteristics of solar atmosphere plasma in these areas were found using solar images, taken with Extreme ultraviolet Imaging Telescope (EIT) onboard SOHO.
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