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J.G. Jernigan (UCB)
We present a new model for kHz QPO observed in LMXB sources which relates the uniform properties of these emissions over a wide range of accretion rates to the intrinsic properties of neutron star (NS) structure. This model is in strong contrast to existing models which primarily relate the kHz QPO phenomenon to the physics of gas dynamics near the inner edge of the accretion disk and the transition flow onto the surface of the NS. Comparison of the observations with the new model places strong constraints on the equation of state of NS matter. We also predict gravitational wave emission of a consequence of the new model.