Observational Determination of the Rate of Magnetic Helicity Transport through the Solar Surface via the Horizontal Motion of Field Line Footpoints

By J. Chae. 2001

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Photospheric flux density of magnetic helicity (2005, methodology): “All previous analyses used the density GA (= − 2(A · u)Bn) which involves the vector potential A of the magnetic field (Chae 2001; Chae et al. 2001, 2004; Kusano et al. 2002, 2005; Nindos & Zhang 2002; Nindos et al. 2003; Moon et al. 2002a,b).”
Tracking Vector Magnetograms with the Magnetic Induction Equation (2008, methodology): “In the best-case scenarios only the shearing fluxes are captured by line-of-sight tracking methods in partial agreement with the Ansatz of Chae (2001) and in disagreement with the geometrical arguments of Démoulin & Berger (2003) who argue that line-ofsight tracking methods capture both the…”
Solar Surface Emerging Flux Regions: A Comparative Study of Radiative MHD Modeling and Hinode SOT Observations (2008, methodology): “In accordance with our periodic side boundary conditions, we use Fourier transforms (cf. Chae 2001) to calculate ~Ap for a given Bz distribution.”
Physics of Solar Prominences: II—Magnetic Structure and Dynamics (2010, background): “10) generally invoke reconnection low in the solar atmosphere as the pivotal cause of mass at prominence temperatures being expelled into the corona (Wang, 1999; Chae, 2001).”