  Since the discovery of pulsars, the rotating-lighthouse model has been the
choice of model to explain the radiation pulsation of pulsars. After
discovering that some main sequence stars (e.g., CU Virginis) and ultracool
dwarfs (e.g., TVLM 513-46546) also behave like pulsars, the lighthouse model
was again adopted to explain their pulse signals. Our research found that if we
use the magnetic-field oscillation (MO) model, we can explain the pulse
radiation results better regardless of whether its source is a neutron star, a
main-sequence star or an ultracool dwarf. We propose a verifiable prediction
that can be used to evaluate the MO model. Our prediction is that there is a 90
degree phase lag between the magnetic field and radio signal of TVLM 513-46546,
and the zero-crossing point of the magnetic field is the moment when the
direction of the light's circular polarization is reversed. No new observations
are needed to check this prediction, but certain existing data needs to be
re-mined.
