Magnetohydrodynamic simulations of A-type stars: Long-term evolution of core dynamo cycles

Open Access

Fig. 8.

Profiles of the temporally and azimuthally averaged rotation rate, $\bar{Ω} (ϖ, z),$ $\overline{\Omega}(\varpi,z),$ of selected runs from all sets (clipped at r = 0.5R). The upper panels show all the runs with P_rot = 15 days (MHDr2, MHDr2*, and zMHDr2). The lower panels shows the run with no dynamo (MHDr1), and two simulations with P_rot = 8 days (MHDr4 and MHDr4*).

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