  We constructed the magnetic field oscillation model (hereafter the MO model)
by analogizing the periodically reversing phenomenon of the solar magnetic
field to pulsars. Almost all kinds of pulsar radiation phenomena are best
explained using the MO model, especially polarization characteristics, glitch,
generation rate, the geodetic precession of pulsars and the configuration of
pulsar-wind nebula of the Crab. The MO model also provides satisfactory
explanation for other characteristics of pulsars, e.g., interpulse, spin-down,
pulse nulling, beat and pulse drift, the loss rate of the rotating energy, and
the accuracy of frequency. We present eight verification methods for the MO
model. In addition to pulsars, our MO model can also be used to explain the
pulse emission from non-compact stars such as the ultracool dwarf TVLM
513-46546 and the magnetic chemically peculiar star CU Virginis.
