Signatures of hadron-quark mixed phase in gravitational waves

We calculate stellar oscillations, including the hadron-quark mixed phase, considering finite-size effects. We find that it is possible to distinguish whether the density discontinuity exists or not in the stars, even if one observes the gravitational waves of the fundamental mode. Additionally, the normalized eigenfrequencies of pressure modes depend strongly on the stellar mass and on the adopted equation of state. In particular, in spite of the fact that the radius of the neutron star with 1.4M(circle dot), which is the standard mass, is almost independent of the equation of state with quark matter, the frequencies of the pressure modes depend on the adopted equation of state. Thus, via observing the many kinds of gravitational waves, it will be possible to make a restriction on the equation of state.