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• W2102165068 abstract "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. The solar wind is basically determined by the Sun's magnetic field and responds in various ways to solar activity and the accompanying changes in the photospheric magnetic field, which determines the coronal magnetic field and therewith the interplanetary magnetic field and solar-wind stream structure in the entire heliosphere. For a modern review of the solar magnetic field see Solanki et al. (2006). The sources of the solar wind are defined by the field, and the origin of the solar wind is closely linked with and influenced by the activity in the magnetic network. As the result of varying boundary conditions in the corona, three basic types of solar wind occur: Fast streams from large coronal holes (CHs); slow streams from small CHs and active regions (ARs), and from the boundary layers of coronal streamers; and the variable transient flows such as coronal mass ejections (CMEs), often associated with eruptive prominences, or plasmoids stemming from the top of streamers, and other ejections from ARs driven through magnetic reconnection. These basic types of solar wind are closely associated with the structure and the activity of the coronal magnetic field (for recent reviews see, e.g., Marsch, 2006, and Schwenn, 2006) that changes over the solar cycle. This paper gives a concise review of the origin of the solar wind, with emphasis on the magnetic nature of the source regions, as they become evident in the solar extreme ultraviolet (EUV) emission patterns and in coronagraph images. The plasma characteristics as well as the magnetic structures 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, in particular at small scales, and discussed from the observational point of view. 2. Dynamic magnetic network The Sun's magnetic field together with the plasma properties and processes in its lower atmosphere, such as photospheric convection, temperature distribution, density stratification, current sheets and plasma waves, largely determine the origin and evolution of the solar wind." @default.
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• W2102165068 date "2006-01-01" @default.
• W2102165068 modified "2023-09-27" @default.
• W2102165068 title "Coronal origins of the solar wind - sources of steady streams and transient flows caused by solar magnetic eruptions" @default.
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