Influence of Magnetic Diffusion on Short-Wavelength Magnetic Buoyancy Instability

etc15 Tracking Number 344

Magnetic buoyancy instability (MBI) is believed to plays an important role in the evolution of magnetic fields in astrophysical objects. In the Sun large-scale toroidal magnetic field is probably generated in the tachocline – a thin region of strong radial shear, between radiative and convective zones. Observations indicate that this field rises the surface and create active regions. MBI is a probable mechanism for this phenomenon. Magnetic and thermal diffusivity are parameters of solar plasma which could be important for dynamics of MBI. Here we consider preliminary case which include only magnetic dissipation. The singular perturbation methods are used to find difference with case without any dissipation.