Abstract
We present a contemporary view of how solar active region magnetic fields are understood to be generated, transported and dispersed. Empirical trends of active region properties that guide model development are discussed. Physical principles considered important for active region evolution are introduced and advances in modeling are reviewed.
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Acknowledgements
MCMC is supported by NASA’s SDO/AIA contract (NNG04EA00C) and grant (NNX13AJ96G) to LMSAL. AIA is an instrument onboard the Solar Dynamics Observatory, a mission for NASA’s Living With a Star program. Part of this paper was written while MCMC was a Visiting Associate Professor at the National Astronomical Observatory of Japan (NAOJ) in Tokyo. MCMC wishes to thank his NAOJ hosts, especially Professor Shin Toriumi, for their excellent hospitality. LvDG acknowledges the Hungarian Scientific Research Fund (OTKA) for support through grant no. K-109276. The National Solar Observatory is operated by AURA, Inc. under a cooperative agreement with the National Science Foundation. The National Center for Atmospheric Research is sponsored by the National Science Foundation. Finally, the authors wish to thank the anonymous referee for very constructive feedback.
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Cheung, M.C.M., van Driel-Gesztelyi, L., Martínez Pillet, V. et al. The Life Cycle of Active Region Magnetic Fields. Space Sci Rev 210, 317–349 (2017). https://doi.org/10.1007/s11214-016-0259-y
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DOI: https://doi.org/10.1007/s11214-016-0259-y