Coronal origins of the solar wind - sources of steady streams and transient flows caused by solar magnetic eruptions

The magnetic field of the Sun and the plasma properties of its atmosphere, such as temperature distribution, density stratification, photospheric convection and waves in the corona, determine the origin, energetics and evolution of the solar wind. The solar wind comes in three main kinds, as steady fast streams, variable slow flows and transient slow and fast coronal mass ejections. The three types of solar wind are closely associated with the structure and activity of the coronal magnetic field. The plasma characteristics and magnetic features of the solar wind source regions are reviewed. The boundary conditions in the mostly closed corona (streamers and loops), in the transiently opening corona (eruptive prominences and loops) and in the lastingly open corona (funnels and holes) will be analyzed. The resulting properties of the solar wind are discussed.