  Recent observations of coronal-loop waves by TRACE and within the corona as a
whole by CoMP clearly indicate that the dominant oscillation period is 5
minutes, thus implicating the solar p modes as a possible source. We
investigate the generation of tube waves within the solar convection zone by
the buffeting of p modes. The tube waves--in the form of longitudinal sausage
waves and transverse kink waves--are generated on the many magnetic fibrils
that lace the convection zone and pierce the solar photosphere. Once generated
by p-mode forcing, the tube waves freely propagate up and down the tubes, since
the tubes act like light fibers and form a waveguide for these magnetosonic
waves. Those waves that propagate upward pass through the photosphere and enter
the upper atmosphere where they can be measured as loop oscillations and other
forms of propagating coronal waves. We treat the magnetic fibrils as vertically
aligned, thin flux tubes and compute the energy flux of tube waves that can
generated and driven into the upper atmosphere. We find that a flux in excess
of 10^5 ergs/cm^2/s can be produced, easily supplying enough wave energy to
explain the observations. Furthermore, we compute the associated damping rate
of the driving p modes and find that the damping is significant compared to
observed line widths only for the lowest order p modes.
