Polarization is a measure of the way in which light or other electromagnetic radiation from a celestial body is affected by factors such as scattering due to cosmic dust or strong stellar or interstellar magnetic fields, or reflection from a surface. Radio emissions from celestial sources are usually partially polarized, i.e. the waves can be considered to be composed of a completely unpolarized component plus a small polarized component. Synchrotron emission, however, may be strongly polarized. The general situation is described by the four Stokes parameters (I, Q, U, and V ), which are defined in such a manner that specifying their four values uniquely describes the state of polarization: I is a measure of the total power in the wave, Q and U define the degree of linear polarization, and V that of circular polarization. All four have dimensions of flux density. See also Faraday rotation; interstellar polarization.