The third-generation gravitational wave (GW) detectors will further enhance our ability to detect GW signals. However, we are still uncertain about their performance in some specific frequency bands, especially for the detection of GWs in the kilohertz (kHz) frequency range. In this study, we simulate 1000 events of 1.4M⊙–1.4M⊙ binary neutron star (BNS) mergers with an upper limit of redshift at z = 1.4, and evaluate the detection capabilities of the third-generation detectors like Cosmic Explorer (CE), Einstein Telescope (ET), as well as the potential kHz detector that may be built in China in the future. Their detection rates for those simulated events reach 61.3%, 100%, and 32.4%, respectively. Additionally, we compare the signal-to-noise ratios (SNRs) of the three detectors in different frequency ranges  divided by different fmid values. When fmid is greater than 70 Hz, the kHz detector begins to show an advantage over CE in a specific redshift range. While for ET, fmid needs to be greater than 1480 Hz. Moreover, as fmid takes its maximum value of 4500 Hz, in this frequency band, the kHz detector has the greatest advantage in detecting BNS merger events at z = 0.46 and z = 0.47, with its SNR being 4.3 and 2.8 times that of CE and ET, respectively. For signals in the frequency band  of the post-merger phase, compared to the other two detectors, the kHz detector can achieve results that are 4.1 times and 2.7 times higher for sources located at z = 0.35 and z = 0.36, respectively. These results indicate that the kHz detector is more sensitive to high-frequency GWs than CE and ET, and it may play a crucial role in capturing the details of the post-merger phase of BNS mergers, which is difficult to observe with existing or other instruments primarily focused on low-frequency GW signals.

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