Turbulent and directed mass motions in various structures of the low corona

1. Introduction

[2] The presence of large velocities in the low corona (up to heights h sim 1.2--1.5 R ) was long ago known from ground-based observations. The spacecraft data obtained in the last decades, especially in the far UV from the ESA/NASA Solar and Heliospheric Observatory (SOHO), have clearly demonstrated that the low layers of the solar corona are much more dynamic than it was supposed before. In this review we have collected information about turbulent and directed velocities in various structural formations and in the quiet (diffuse) corona. We have used the results from published papers, based both on the ground and space observations in visual and ultraviolet spectral regions and our observations of four eclipses.