  Many models for the pulsar radio and $\gamma$-ray emissions have been
developed. The tests for these models using observational data are very
important. Tests for the pulsar radio emission models using frequency-altitude
relation are presented in this paper. In the radio band, the mean pulse
profiles evolve with observing frequencies. There are various styles of pulsar
profile - frequency evolutions (which we call as "beam evolution" figure), e.g.
some pulsars show that mean pulse profiles are wider and core emission is
higher at higher frequencies than that at lower frequencies, but some other
pulsars show completely the contrary results. We show that all these "beam
evolution" figures can be understood by the Inverse Compton Scattering(ICS)
model (see Qiao at al.2001 also). An important observing test is that, for a
certain observing frequency different emission components are radiated from the
different heights. For the $\gamma$-ray pulsars, the geometrical method (Wang
et al. 2006) can be used to diagnose the radiation location for the
$\gamma$-ray radiation. As an example, Wang et al. (2006) constrain the
$\gamma$-ray radiation location of PSR B1055-52 to be the place near the null
charge surface. Here we show that Wang's result matches the proposed radiation
locations by the annular gap model as well as the outer gap models.
