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Context: Subdwarf B stars (sdBs) play a crucial role in stellar evolution,asteroseismology, and far-UV radiation of early-type galaxies, and have beenintensively studied with observation and theory. It has theoretically beenpredicted that sdBs with neutron star (NS) companions exist in the Galaxy, butnone have been discovered yet. This remains a puzzle in this field. In aprevious study (hereafter Paper I), we have studied the formation channels ofsdB+NS binaries from main-sequence (MS) stars plus NS binaries by establishinga model grid, but it is still unclear how these binaries consisting of MS starsand NS binaries came to be in the first place. Aims: We systematically studythe formation of sdB+NS binaries from their original zero-age main-sequenceprogenitors. We bridge the gap left by our previous study in this way. Weobtain the statistical population properties of sdB+NS binaries and providesome guidance for observational efforts. Methods: We first used Hurley's rapidbinary evolution code BSE to evolve 10^7 primordial binaries to the point wherethe companions of NS+MS, NS+Hertzsprung gap (HG) star, and NS+Giant Branch (GB)star binaries have just filled their Roche lobes. Next, we injected thesebinaries into the model grid we developed in Paper I to obtain the propertiesof the sdB+NS populations. We adopted two prescriptions of NS natal kicks.Different values of common-envelope ejection efficiency were chosen to examinethe effect of common-envelope evolution on the results. Conclusions: MostsdB+NS binaries are located in the Galactic disk with small RV semi-amplitudes.SdB+NS binaries with large RV semi-amplitudes are expected to be strong GWRsources, some of which could be detected by LISA in the future.

Hot subdwarf B stars with neutron star components II: Binary population synthesis