  We compute the 20 lowest frequency radial oscillation modes of strange stars
admixed with condensed dark matter. We assume a self-interacting bosonic dark
matter, and we model dark matter inside the star as a Bose-Einstein condensate.
In this case the equation of state is a polytropic one with index $1+1/n=2$ and
a constant $K$ that is computed in terms of the mass of the dark matter
particle and the scattering length. Assuming a mass and a scattering length
compatible with current observational bounds for self-interacting dark matter,
we have integrated numerically first the Tolman-Oppenheimer-Volkoff equations
for the hydrostatic equilibrium, and then the equations for the perturbations
$\xi=\Delta r/r$ and $\eta=\Delta P/P$. For a compact object with certain mass
and radius we have considered here three cases, namely no dark matter at all
and two different dark matter scenarios. Our results show that i) the
separation between consecutive modes increases with the amount of dark matter,
and ii) the effect is more pronounced for higher order modes. These effects are
relevant even for a strange star made of 5\% dark matter.
