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We infer the emission positions of twin kilohertz quasi-periodic oscillations(kHz QPOs) in neutron star low mass X-ray binaries (NS-LMXBs) based on theAlfven wave oscillation model (AWOM). For most sources, the emission radii ofkHz QPOs cluster around a region of 16-19 km with the assumed NS radii of 15km. Cir X-1 has the larger emission radii of 23-38 km than those of the othersources, which may be ascribed to its large magnetosphere-disk radius or strongNS surface magnetic field. SAX J1808.4-3658 is also a particular source withthe relative large emission radii of kHz QPOs of 20 - 23 km, which may be dueto its large inferred NS radius of 18 - 19 km. The emission radii of kHz QPOsfor all the sources are larger than the NS radii, and the possible explanationsof which are presented. The similarity of the emission radii of kHz QPOs (16-19km) for both the low/high luminosity Atoll/Z sources is found, which indicatesthat both sources share the similar magnetosphere- disk radii.

Investigation of the emission radii of kHz QPOs for the accreting millisecond X-Ray pulsars, Atoll and Z sources