Emission from pulsars. I. A generalized single-vector polarization model. II. A model for the sub-pulse and integrated pulse behavior

In Part I, the properties of models for pulsar polarization which incorporate localized emission regions corotating with a neutron star are investigated. The formulae applicable to the case where emission comes from near the neutron star surface are derived and compared with those applicable for emission from further out in the magnetosphere. In all the models investigated, it is assumed that the instantaneous polarization position angle is given by the apparent projection of a corotating magnetic field vector on the plane of the sky, and that the percentage of linear polarization is proportional to some power of the apparent projected length of the vector along the line of sight. Relativistic effects which become important for emission from far out in the magnetosphere are thoroughly discussed and related to the polarization behavior predicted by the models. In Part II, the pulsar observations believed important for an understanding of their physical nature are discussed. Pulsar PSR 0329 + 54 provides a detailed look at properties of a typical pulsar. It is shown that if the radiation is cyclotron or single electron synchrotron radiation then the emission frame is in rapid motion relative to the observer. Possible mechanisms for producing broad band individual pulse (sub-pulse) radiation are discussed. Also, the relativistic vector model is fit to several pulsars which represent different classes in a popular classification scheme. The Crab Nebula pulsar is discussed in detail. Finally, guidelines for possible theoretical models of the emission are presented.