Abstract
The Einstein-Maxwell field equations for a charged perfect-fluid distribution in a stationary axisymmetric space-time are investigated. Under the assumption of slow rotation, these equations have been reduced to represent slowly rotating charged fluid spheres. It is observed that, similar to the case of slowly rotating uncharged fluid spheres, the field equations split into two parts: viz., the field equations for a static charged fluid sphere and the equations that determine the parameters \ensuremath{\omega} and \ensuremath{\Omega} which represent the angular velocity of the fluid distribution and the angular velocity of the inertial frames along the rotation axis, respectively.
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