The effect of local magnetic fields in quiet regions of stellar atmospheres simulated with MANCHA

Open Access

Fig. 16

Magnetic energy averaged over surfaces of constant geometrical height and time from the SSD runs (black lines), compared to the difference in kinetic (top row) and internal (bottom) energy (Eq. (9) multiplied by –1; red lines) between the HD and SSD runs. Shaded areas show $σ / \sqrt{N}$ $\sigma /\sqrt N$ for the magnetic energy and the error (Eq. (3)) for the difference of energy between the SSD and HD cases.

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