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The mass ($M_{\rm TOV}$) and radius ($R_{\rm TOV}$) of the maximum-massnonrotating neutron star (NS) play a crucial role in constraining the elusiveequation of state of cold dense matter and in predicting the fate of remnantsfrom binary neutron star (BNS) mergers. In this study, we introduce a novelmethod to deduce these parameters by examining the mergers of second-generation(2G) black holes (BHs) with NSs. These 2G BHs are assumed to originate fromsupramassive neutron stars (SMNSs) formed in BNS mergers. Since the propertiesof the remnant BHs arising from the collapse of SMNSs follow a universalrelation governed by $M_{\rm TOV}$ and $R_{\rm TOV}$, we anticipate that byanalyzing a series ($\sim 100$ detections) of mass and spin measurements of the2G BHs using the third-generation ground-based gravitational-wave detectors,$M_{\rm TOV}$ and $R_{\rm TOV}$ can be determined with a precision of $\sim0.01M_\odot$ and $\sim 0.6$ km, respectively.

Measuring Mass and Radius of the Maximum-mass Nonrotating Neutron Star