ABSTRACT
The origin of magnetic activity in the Sun is a fundamental problem of solar magnetohydrodynamics. The magnetic field, as well as being responsible for the solar cycle and the formation of active regions, underlies all solar magnetic phenomena such as solar flares, coronal mass ejections and the solar wind, and is responsible for heating the solar corona to such high temperatures (Tobias, 2002b). Solar magnetic activity is believed to be the result of a hydromagnetic dynamo where inductive motions within the ionized solar plasma are able to generate a magnetic field, overcoming the action of Ohmic dissipation (see, e.g., Weiss, 1994).
