Three-dimensional solar active region magnetohydrostatic models and their stability using Euler potentials

Open Access

Fig. 9.

Non-potential magnetic field lines and isosurfaces calculated numerically by applying transformation on EPs using Eq. (51). Gas pressure and gravity are present. Compare with Fig. 2. In this configuration, a₀ = 0.6, x₀ = 1, w = 1, β₀₀ = 1.4 × 10⁻³, and α_ref = α(−1, 0, 0).

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