  As the hottest high-energy neutrino spot, NGC 1068 has received much
attention in recent years. Here we focus on the central region of the active
galactic nuclei (AGN) and propose an outflow-cloud interaction model that could
probably explain the observed neutrino data. Considering the accretion process
adjacent to the central supermassive black hole (SMBH) of NGC 1068, strong
outflows will be generated, which will likely interact with surrounding clouds
floating in the corona region. Particles carried by the outflow will be
accelerated to very high energy by the shocks forming during the outflow-cloud
interactions. For the accelerated high-energy protons, $p\gamma$ interactions
with the background photon field of the corona and disk and $pp$ interaction
with the surrounding gas will produce considerable high-energy $\gamma$-rays
and neutrino. However, because of the extremely dense photon fields in the
corona and disk, the newly generated $\gamma$-rays will be significantly
attenuated through the $\gamma\gamma$ absorptions. In our scenario, the
expected GeV-TeV $\gamma$-ray emission will be suppressed to a much lower level
than the neutrino emission, consistent with the observational characteristics
of NGC 1068, while the generated 1-30\,TeV neutrino flux can fit the IceCube
data very well.
