  We discover three new weak pulse components in two known pulsars, one in PSR
J0304+1932 and two in PSR J1518+4904. These components are emitted about half
way between the main emission beam and the interpulse beam (beam from the
opposite pole). They are separated from their main pulse peak by
$99^{\circ}\pm{3}^{\circ}$ for J0304+1932, $123^{\circ}.6\pm{0^{\circ}.7}$
(leading) and $93^{^{\circ}}\pm 0^{\circ}.4$ (trailing) for J1518+4904,
respectively. Their peak-intensity ratios to main pulses are: $\sim$ 0.06% for
J0304+1932, $\sim$ 0.17% and $\sim$ 0.83% for J1518+4904. We also analyzed flux
fluctuation and profile variation of the emissions for two pulsars. The results
show correlations between the weak pulses and their main pulses, indicating
that these emissions come from the same pole. We estimated the emission
altitude of these weak pulses and derived a height of about half of the
pulsar's light-cylinder radius. These pulse components are a unique sample of
high-altitude emissions from pulsars, and challenge the current pulsar emission
models.
