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Paper: Numerical Simulation and SOT Magnetogram Analysis of the Small-scale Magnetic Elements in a Solar Emerging Flux Region
Volume: 456, The Fifth Hinode Science Meeting
Page: 33
Authors: Toriumi, S.; Yokoyama, T.
Abstract: In this study, we aim to figure out the flux emergence from the interior to the atmosphere through the surface, by conducting a numerical simulation and a Hinode/SOT observation. First, we performed a three-dimensional magnetohydrodynamic (MHD) simulation on the flux tube emergence from –20,000 km of the convective layer. As a result, the rising tube expands sideways beneath the surface to create a flat structure. As time goes on, the subphotospheric field rises again into the corona due to the magnetic buoyancy instability. We newly found that the photospheric magnetogram shows multiple separation events as well as shearing motions, which reflects the Parker instability of the subphotospheric field. This situation agrees well with Strous & Zwaan (1990)'s model based on their observation. We also confirmed that the wavelength perpendicular to the separations is approximately a few times the tube's initial radius. Secondly, we analyzed SOT/FG magnetogram of AR 10926, and observed that the small-scale magnetic elements among the major sunspots make alignments with a certain orientation. The wavelength perpendicular to the alignments was found to be ∼3,000km. Comparing with the numerical results, we speculate that this active region observed by the SOT is created by the rising flux tube with a radius of the order of 1,000 km in the deeper convection zone.
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