Fluctuation structure of pulsar pulses scattered by a turbulent interstellar phase screen

After a narrow, coherent radiation pulse has been scattered by a turbulent layer it will form a strain of subpulses whose envelope is described by the expression for the average shape of the scattered pulse; the characteristic width of an individual subpulse will be equal to the width of the initial pulse. If the original radiation has a wide bandwidth, the fluctuation microstructure of the pulse can only be detected if the receiver bandwidth is matched to the time scale of the initial pulse such that their product is less than or equal to 1. It should be possible to measure the pulse microstructure parameters even for features smaller than the average broadening caused by interstellar scattering.