ShearAlfvén

shearAlfvén is a type of magnetohydrodynamic (MHD) wave that propagates in a magnetized plasma. These waves are characterized by the displacement of plasma perpendicular to both the ambient magnetic field and the direction of wave propagation. The restoring force for shearAlfvén waves comes from the tension in the magnetic field lines. When a portion of the plasma is displaced perpendicular to the magnetic field, the magnetic field lines are bent, creating a magnetic tension that pulls the plasma back towards its equilibrium position. This oscillation propagates along the magnetic field lines.

The speed at which shearAlfvén waves travel is known as the Alfvén speed. This speed is dependent on the strength of the magnetic field and the density of the plasma. Specifically, the Alfvén speed is proportional to the square root of the magnetic field strength divided by the plasma density. ShearAlfvén waves are transverse waves, meaning the plasma particles oscillate perpendicular to the direction of wave propagation. Unlike compressional waves, shearAlfvén waves do not involve significant changes in plasma pressure or density. They are fundamental to understanding various phenomena in space plasmas, such as solar flares, coronal heating, and the dynamics of planetary magnetospheres. They can also play a role in laboratory plasmas.