Theories of the solar cycle: a critical view

Some established views of the solar magnetic cycle are discussed crit-ically, with focus on two aspects at the core of most models: the role of convective turbulence, and the role of the ‘tachocline ’ at the base of the con-vection zone. The standard view which treats the solar cycle as a manifes-tation of the interaction between convection and magnetic fields is shown to be misplaced. The main ingredient of the solar cycle, apart from differential rotation, is instead buoyant instability of the magnetic field itself. This view of the physics of the solar cycle was already established in the 1950s, but has been eclipsed mathematically by mean field turbulence formalisms which make poor contact with observations and have serious theoretical problems. The history of this development in the literature is discussed critically. The source of the magnetic field of the solar cycle is currently assumed to be lo-cated in the ‘tachocline’: the shear zone at the base of the convection zone. While the azimuthal field of the cycle is indeed most likely located at th