  R-mode instabilities lead to specific signatures in the evolution of rotating
pulsars, and may provide a unique signature which can identify the phase of
matter that exists in the interiors of such objects.
  The contributions of quarks' bulk and shear viscosities to the dissipation of
r-mode instabilities are studied. It is shown that (contrary to earlier works)
the quark contribution is \emph{not} fully suppressed in the presence of fully
gapped color-superconducting phase due to the fact that the bulk viscosity is a
resonance effect between the density oscillation on one side, and the
interaction rates that try to restore $\beta$-equilibrium during these
oscillations on the other. This will have an effect on the structure of the
r-mode instability window and will affect the angular momentum evolution of
pulsars.
