Impacts of small-scale dynamo on rotating columnar convection in stellar convection zones

Open Access

Fig. 19.

(Top) Correlations between the Maxwell stress, $\tilde{B_{x} B_{z}} / 4 π$ $\widetilde{B_x B_z} / 4\pi$ , and the Reynolds stress, $ρ_{0} \tilde{v'_{x} v'_{z}}$ $\rho_0 \widetilde{v\prime_x v\prime_z}$ , and (bottom) correlations between $\tilde{B_{x} B_{z}} / 4 π$ $\widetilde{B_x B_z} / 4\pi$ and the velocity strain tensor, $ρ_{0} {\tilde{S}}_{xz} = ρ_{0} (\partial_{z} \tilde{v}'_{x} + \partial_{x} \tilde{v}'_{z})$ $\rho_0 \widetilde{\mathcal{S}}_{xz}= \rho_0 (\partial_z \widetilde{v}\prime_x + \partial_{x} \widetilde{v}\prime_z)$ , in MHD simulations. (a,b) Probability density functions (PDFs) between $\tilde{B_{x} B_{z}} / 4 π$ $\widetilde{B_x B_z} / 4\pi$ and $ρ_{0} \tilde{v'_{x} v'_{z}}$ $\rho_0 \widetilde{v\prime_x v\prime_z}$ in MHD-Co2 and MHD-Co20 cases. (c) Correlation coefficient as a function of Co_*. (d,e) PDFs between $\tilde{B_{x} B_{z}} / 4 π$ $\widetilde{B_x B_z} / 4\pi$ and $ρ_{0} {\tilde{S}}_{xz}$ $\rho_0 \widetilde{\mathcal{S}}_{xz}$ in MHD-Co2 and MHD-Co20 cases. (f) Correlation coefficients $\tilde{B_{x} B_{z}} / 4 π$ $\widetilde{B_x B_z} / 4\pi$ vs. $ρ_{0} {\tilde{S}}_{xz}$ $\rho_0 \widetilde{\mathcal{S}}_{xz}$ (purple) and $ρ_{0} \tilde{v'_{x} v'_{z}}$ $\rho_0 \widetilde{v\prime_x v\prime_z}$ vs. $- ρ_{0} {\tilde{S}}_{xz}$ $-\rho_0 \widetilde{\mathcal{S}}_{xz}$ (green) as functions of Co_*. The dashed and solid green lines show the results from HD and MHD simulations, respectively.

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