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• W4386119095 abstract "Aims. The aim of this study is to explore the magnetic and flow properties of fully convective M dwarfs as a function of rotation period P rot and magnetic Reynolds Re M and Prandlt numbers Pr M . Methods. We performed three-dimensional simulations of fully convective stars using a star-in-a-box set-up. This set-up allows global dynamo simulations in a sphere embedded in a Cartesian cube. The equations of non-ideal magnetohydrodynamics were solved with the P ENCIL C ODE . We used the stellar parameters of an M5 dwarf with 0.21 M ⊙ at three rotation rates corresponding to rotation periods ( P rot ) of 43, 61, and 90 days, and varied the magnetic Prandtl number in the range from 0.1 to 10. Results. We found systematic differences in the behaviour of the large-scale magnetic field as functions of rotation and Pr M . For the simulations with P rot = 43 days and Pr M ≤ 2, we found cyclic large-scale magnetic fields. For Pr M > 2, the cycles vanish and the field shows irregular reversals. In the simulations with P rot = 61 days for Pr M ≤ 2, the cycles are less clear and the reversal are less periodic. In the higher Pr M cases, the axisymmetric mean field shows irregular variations. For the slowest rotation case with P rot = 90 days, the field has an important dipolar component for Pr M ≤ 5. For the highest Pr M the large-scale magnetic field is predominantly irregular at mid-latitudes, with quasi-stationary fields near the poles. For the simulations with cycles, the cycle period length slightly increases with increasing Re M ." @default.
• W4386119095 created "2023-08-25" @default.
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• W4386119095 date "2023-10-01" @default.
• W4386119095 modified "2023-10-16" @default.
• W4386119095 title "Simulations of dynamo action in slowly rotating M dwarfs: Dependence on dimensionless parameters" @default.
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• W4386119095 doi "https://doi.org/10.1051/0004-6361/202244666" @default.
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