Abstract
This publication provides an overview of magnetic fields in the solar atmosphere with the focus lying on the corona. The solar magnetic field couples the solar interior with the visible surface of the Sun and with its atmosphere. It is also responsible for all solar activity in its numerous manifestations. Thus, dynamic phenomena such as coronal mass ejections and flares are magnetically driven. In addition, the field also plays a crucial role in heating the solar chromosphere and corona as well as in accelerating the solar wind. Our main emphasis is the magnetic field in the upper solar atmosphere so that photospheric and chromospheric magnetic structures are mainly discussed where relevant for higher solar layers. Also, the discussion of the solar atmosphere and activity is limited to those topics of direct relevance to the magnetic field. After giving a brief overview about the solar magnetic field in general and its global structure, we discuss in more detail the magnetic field in active regions, the quiet Sun and coronal holes.
Highlights
To understand the physical processes in the solar interior, its atmosphere as well as the interplanetary environment, a detailed knowledge of the temporal and spatial properties of the magnetic field is essential
We aimed to review our current understanding of the role of magnetic fields for the physics of the solar atmosphere, in particular the corona
Together with the ever increasing sophistication of numerical techniques, this led to new insights into the nature and the dynamic evolution of the coronal magnetic field
Summary
To understand the physical processes in the solar interior, its atmosphere as well as the interplanetary environment (including “space weather” close to Earth), a detailed knowledge of the temporal and spatial properties of the magnetic field is essential. This is because the magnetic field is the link between everything, from the Sun’s interior to the outer edges of our solar system. We aim to give an overview of the magnetic coupling from the solar surface to the Sun’s upper atmosphere, with special emphasis on the structure and evolution of the coronal magnetic field. Abbreviations used throughout this manuscript are defined in Appendix 8
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