Parker Instability is an instability caused by magnetic buoyancy. The magnetic field observed on the solar surface is considered that magnetic field greated inside of the Sun emerges by magnetic buoyant instability.

[Initial Condition]

Corresponding to the solar structure, we place photosphere and corona. Pressure equilibrium of gas by constant gravity toward the bottom (negative direction of 'z' axis) of the simulation region is assumed. Amagnetic tube is placed inside the solar surface (at z = 0) and following evolution will be simulated.

In the figure, color shows density, arrows show velocity, and lines show magnetic field lines.

[Evolved Stage]

Magnetic tube will emerge out from the solar surface by magnetic buoyancy.