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We for the first time propose a physical model of the precursor (PR) andinterpulse (IP) components of the radio pulsar profiles. It is based onpropagation effects in the secondary plasma flow of a pulsar. The componentsare suggested to result from the induced scattering of the main pulse (MP) intobackground. The induced scattering appears efficient enough to transfer asignificant part of the MP energy to the background radiation. In the regimesof superstrong and moderately strong magnetic field, the scattered componentsare approximately parallel and antiparallel to the velocity of the scatteringparticles and can be identified with the PR and IP, respectively. The spectralevolution, polarization properties, and fluctuation behaviour of the scatteredcomponents are examined and compared with the observational results. Theperspectives of the complex profile studies are outlined as well.

Physics of pulsar radio emission outside of the main pulse