  The dense wind environment (or circumstellar medium) may be ubiquitous for
the regular Type II supernovae (SNe) before the explosion, the interaction of
which with the SN ejecta could result in a wind breakout event. The shock
generated by the interaction of the SN ejecta and the wind can accelerate the
protons and subsequently the high-energy gamma-rays and neutrinos could arise
from the inelastic pp collisions. In this work, we present the detailed
calculations of gamma-ray and neutrino production for the regular Type II SNe.
The calculation is executed by applying time-dependent evolutions of dynamic
and proton distribution so that the emission could be shown at different times.
Our results show, for the SN 2013fs-like wind environment, the multi-GeV and ~
few-100 TeV gamma-rays are detectable with a time window of several days at <~
2-3 Mpc by Fermi/LAT and CTA during the ejecta-wind interaction, respectively,
and can be detected at a further distance if the wind environment is denser.
Besides, we found the contribution of the wind breakouts of regular Type II SNe
to diffuse neutrino flux is subdominant by assuming all Type II SNe are SN
2013fs-like, whereas for a denser wind environment the contribution could be
conspicuous above 300TeV.
