Abstract
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.
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Acknowledgements
The authors would like to thank the anonymous referee for their careful reading and constructive criticism. This work received generous support from the National Natural Science Foundation of China, Project Nos 11763007, 11863005, 11803026 and 11503008. They would also like to express their sincere gratitude to the Tianshan Youth Project of Xinjiang No. 2018Q014.
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Nurmamat, N., Zhu, C., Lü, G. et al. Quark novae: An alternative channel for the formation of isolated millisecond pulsars. J Astrophys Astron 40, 32 (2019). https://doi.org/10.1007/s12036-019-9596-z
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DOI: https://doi.org/10.1007/s12036-019-9596-z