  We present magnetohydrodynamic simulations of a jet-wind interaction in a
galaxy cluster and the radio to gamma-ray and the neutrino emissions from this
"head-tail galaxy". Our simulation follows the evolution of cosmic-ray (CR)
particle spectra with energy losses and the stochastic turbulence acceleration.
We find that the reacceleration is essential to explain the observed radio
properties of head-tail galaxies, in which the radio flux and spectral index do
not drastically change. Our models suggest that hard X-ray emissions can be
detected around the head-tail galaxy in the Perseus cluster by the hard X-ray
satellites, such as FORCE, and it will potentially constrain the acceleration
efficiency. We also explore the origin of the collimated synchrotron threads,
which are found in some head-tail galaxies by recent high-quality radio
observations. Thin and elongated flux tubes, connecting the two tails, are
formed by strong backflows at an early phase. We find that these threads advect
with the wind for over 300 Myr without disrupting. The radio flux from the flux
tubes is much lower than the typical observed flux. An efficient CR diffusion
process along the flux tubes, however, may solve this discrepancy.
