Magnetic flux cancellation in a flux-emergence magnetohydrodynamics simulation of coronal hole eruptions and jets

Open Access

Fig. 9.

S-shaped magnetic field lines of Fig. 8 coloured as a function of $V_{z}^{⊥}$ $V_{z}^{\perp }$ (upper row) and κ_z (lower row) along their lengths for time-step 42. The left (right) column corresponds to overhead (side) views.

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