Dynamo simulations of geodynamo, solar dynamo, and VKS experiment are quite difficult due to their complex geometries and the low magnetic Prandtl number of the fluid. Glatzmaier and Roberts [8] simulated geodynamo in the spherical geometry and observed reversals for the first time. A large number of numerical simulations however focus on box simulations with specialised forcing such as Taylor-Green, ABC, and Roberts. These studies attempt to derive conditions for dynamo, such as minimum magnetic Reynolds number (Rc M) and Prandtl number (Pc M). In the present paper we will focus on Taylor-Green (TG) dynamo which is quite popular. For TG forcing, Ponty et al. [3] reported that Rc M increases sharply with P−1 M as turbulence sets in, and then it saturates (see Fig. 3). Mininni et al. [9] and Yadav et al. [10] observed interesting spatial structures in TG dynamo
Dynamo simulations of geodynamo, solar dynamo, and VKS experiment are quite difficult due to their complex geometries and the low magnetic Prandtl number of the fluid. Glatzmaier and Roberts [8] simulated geodynamo in the spherical geometry and observed reversals for the first time. A large number of numerical simulations however focus on box simulations with specialised forcing such as Taylor-Green, ABC, and Roberts. These studies attempt to derive conditions for dynamo, such as minimum magnetic Reynolds number (Rc M) and Prandtl number (Pc M). In the present paper we will focus on Taylor-Green (TG) dynamo which is quite popular. For TG forcing, Ponty et al. [3] reported that Rc M increases sharply with P−1 M as turbulence sets in, and then it saturates (see Fig. 3). Mininni et al. [9] and Yadav et al. [10] observed interesting spatial structures in TG dynamo
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