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For an ordinary class of neutron stars whose compactness is large, the damping rate of some of relatively lower w modes is certainly smaller than that of (Formula presented) modes 7. Thus, only about the detection of them, the w modes would be more significant than the (Formula presented) modes in this class of neutron stars. For the models of the quark star adopted in this work, however, all damping rates of w modes are larger than that of the lowest (Formula presented) mode, because the compactness is smaller than that of such neutron stars 44. This tendency is discussed and clearly stated in Ref. 44. Therefore, we investigate the parameter dependence of the (Formula presented) modes for our current purposes
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