To investigate a dynamic process responsible for flux cancellation
in a solar surface, we performed a three-dimensional MHD simulation of flux emergence, in which surface dynamics and magnetism are reproduced self-consistently via emergence of a magnetic flux tube from a solar interior to the surface. When magnetic field lines composing the flux tube emerge in the shape of Ω (Ω-loop of concave-down geometry), a dense plasma drains down along legs of an Ω-loop to make it rise naturally. On the other hand, when a U-loop of concave-up geometry that underlies an axis of the flux tube has a dip below the surface and
a local peak somewhere above the surface on either side of the dip, it does not emerge easily because
the dense plasma tends to accumulate at the dip, even if emergence of the U-loop could produce
flux cancellation. However, a certain type of U-loop does emerge when one of the local peaks is sufficiently low,
existing about an order of photospheric gas pressure scale height above the surface. In this case the accumulated plasma drains out of the dip by a siphon-like mechanism, allowing the dip to emerge and producing flux cancellation (U-loop emergence-based flux cancellation; this is a formula for estimating the rate of canceling flux via U-loop emergence). In contrast to that, when both local peaks of a U-loop exist much higher than the pressure scale height above the surface, the accumulated plasma simply settles at the dip to prevent it from emerging. Rather, deep dip structure (V-loop) develops via submergence of the U-loop, where
magnetic reconnection could occur to annihilate positive and negative magnetic flux (U-loop submergence-based flux cancellation). In summary, PIL-formation via Ω-loop emergence proceeds at an early phase of flux emergence, while U-loop emergence-based flux cancellation and U-loop submergence-based flux cancellation proceed at its intermediate and late phases, respectively.
References
Magara, T., Antiochos, S. K., DeVore, C. R., & Linton, M. G. 2005
, International Scientific Conference on Chromospheric and Coronal
Magnetic Fields, ESA Publication Division, SP-596 p.439-444,
D. Innes, A. Lagg, S. Solanki, D. Danesy (eds.)
Titov, V. S., Priest, E. R., & Démoulin, P. 1993, A&A, 276, 564
Magara, T.
2007 ASPC, 369, 809
Magara, T. 2011 PASJ, 63, 417
Mechanism of W-loop formation
