Abstract
The magnetic structure of the solar corona influences solar activity, including coronal heating and solar flares. Magnetic loops and arcades are observed to dominate the structure of the corona; they are formed by the interaction of high-β photospheric convection with low-β coronal magnetic fields. We show the results of 3-D MHD simulations of the response of coronal fields to convective and shear-flow driving from the photosphere. The principal examples include the micro-flare activity in the Parker loop-heating archetype (Schnack and Mikić 1994), and the formation and revolution of 3-D coronal loops (Van Hoven et al. 1995a).
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van Hoven, G., Mok, Y., Hendrix, D.L., Mikić, Z. (1996). Surface Driven Evolution and Activity of Atmospheric Magnetic Structures. In: Uchida, Y., Kosugi, T., Hudson, H.S. (eds) Magnetodynamic Phenomena in the Solar Atmosphere. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-0315-9_12
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DOI: https://doi.org/10.1007/978-94-009-0315-9_12
Publisher Name: Springer, Dordrecht
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