Quark novae: An alternative channel for the formation of isolated millisecond pulsars

Isolated millisecond pulsars (IMSPs) are a topic of academic contention. There are various models to explain their formation. We explore the formation of IMSP via quark novae (QN). During this formation process, low-mass X-ray binaries (LMXBs) are disrupted when the mass of the neutron star (NS) reaches \(1.8M_\odot \). Using population synthesis, this work estimates that the galactic birthrate of QN-produced IMSPs lies between \({\sim }9.5\times 10^{-6}\) and \({\sim }1.7\times 10^{-4}\) \(\mathrm{yr}^{-1}\). The uncertainties shown in our experiment model is due to the QN’s kick velocity. Furthermore, our findings not only show that QN-produced IMSPs are statistically more significant than those produced by mergers, but also that millisecond pulsar binaries with a high eccentricity may originate from LMXBs that have been involved in, yet not disrupted by, a QN.