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We perform a detailed analysis of the fundamental mode of non-radialpulsations of color flavor locked strange stars. Solving the generalrelativistic equations for non-radial pulsations for an equation of statederived within the MIT bag model, we calculate the frequency and thegravitational damping time of the fundamental mode for all the parametrizationsof the equation of state that lead to self-bound matter.  Our results show that color flavor locked strange stars can emitgravitational radiation in the optimal range for present gravitational wavedetectors and that it is possible to constrain the equation of state'sparameters if the fundamental oscillation mode is observed and the stellar massis determined.  We also show that the $f$-mode frequency can be fitted as a function of thesquare root of the average stellar density $\sqrt{M/R^3}$ by a single linearrelation that fits quite accurately the results for all parametrizations of theequation of state. All results for the damping time can also be fitted as afunction of the compactness $M/R$ by a single empirical relation. Therefore, ifa given compact object is identified as a color flavor locked strange starthese two relations could be used to determine the mass and the radius from theknowledge of the frequency and the damping time of gravitational waves from the$f$ mode.

Constraining color flavor locked strange stars in the gravitational wave era