Abstract
Magnetically, the Sun can be compartmentalized into boxes around active regions that can be modeled separately, since the mean magnetic field strength in the surrounding Quiet Sun regions and in coronal holes is about three orders of magnitude lower. An example of a (dipolar) active region is shown in Fig. 8.1, as observed with HMI/SDO and AIA/SDO in various wavelengths.
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(8.1) Active Regions: Magnetic Field Modeling
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(8.7) Active Regions: Heating
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Aschwanden, M.J. (2019). Active Regions. In: New Millennium Solar Physics. Astrophysics and Space Science Library, vol 458. Springer, Cham. https://doi.org/10.1007/978-3-030-13956-8_8
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