Plasma velocity in hydromagnetic dynamos

Protostellar Disk Dynamos and Hydromagnetic Outflows in Primordial Star Formation

Star formation occurs via accretion through a disk, which is likely to be turbulent, either because of gravitational or magnetorotational instability. Dynamo amplification of magnetic fields needs to be considered. As the disks are also stratified, the turbulence can be helical, with different signs of the helicity in each hemisphere. This provides a key ingredient for amplification of global s...

Resistive and ferritic-wall plasma dynamos in a sphere

Homotopy Analysis Method for Hydromagnetic Plane and Axisymmetric Stagnation-point Flow with Velocity Slip

This work is focused on the steady boundary layer flow near the forward stagnation point of plane and axisymmetric bodies towards a stretching sheet. The no slip condition on the solid boundary is replaced by the partial slip condition. The analytical solutions for the velocity distributions are obtained for the various values of the ratio of free stream velocity and stretching velocity, slip p...

Hydromagnetic Turbulence

Recent progress in astrophysical hydromagnetic turbulence is being reviewed. The physical ideas behind the now widely accepted Goldreich–Sridhar model and its extension to compressible magnetohydrodynamic turbulence are introduced. Implications for cosmic ray diffusion and acceleration is being discussed. Dynamo-generated magnetic fields with and without helicity are contrasted against each oth...

Hydromagnetic turbulence in computer simulations

Hydromagnetic processes play an important role in many astrophysical systems (e.g. stars, galaxies, accretion discs). This is because the medium is hot enough to be partially or fully ionized. Because of the huge scales involved the medium is usually turbulent, provided there is an instability (shear, convection) facilitating the cascading of energy down to small scales. In turbulence research ...