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A statistical model for the polarization of pulsar radio emission is enhancedto account for the heavy modulation of the emission, the possible covariance ofthe Stokes parameters, and the observed asymmetries in the distributions oftotal intensity, polarization, and fractional polarization by treating theintensities of the orthogonal polarization modes as exponential randomvariables. The model is used to derive theoretical distributions to comparewith what is observed. The resulting distributions are unimodal and generallyasymmetric. The unimodality arises from the model's fundamental assumption thatthe orthogonal modes are superposed. The asymmetry originates primarily fromdifferent fluctuations in mode intensities. The distributions of fractionalpolarization are truncated at the degree of linear and circular polarizationintrinsic to the modes. A number of observable parameters that quantify thestatistical properties of the emission and its polarization are derived and areshown to be functions only of the ratio of the modes' mean intensities, M,suggesting their spectra coevolve according to the frequency dependence of M.This particular implementation of the model requires the modes to fluctuatedifferently in order to replicate the observations. Since a single underlyingemission mechanism seems unlikely to selectively modulate the mode intensities,the different fluctuations are attributed either to different emissionmechanisms for the modes or to mode-dependent propagation or scattering effectsin the pulsar magnetosphere.

Exponential Fluctuations in the Modes of Orthogonal Polarization in Pulsar Radio Emission