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

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 1.8 M ⊙ . Using population synthesis, this work estimates that the Galactic birthrate of QN-produced IMSPs lies between ∼ 9.5 × 10 −6 and ∼ 1.7 × 10 −4 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.

A strange star scenario for the formation of eccentric millisecond pulsar PSR J1946+3417

“…By analysing the proper motions of 233 pulsarsHobbs et al (2005) obtained a mean speed of 54(6)kms −1 for recycled pulsars. Employing the rapid binary population synthesis (BPS) code(Hurley et al 2000(Hurley et al , 2002 and a weak kick velocity of σ PT = 60 km s −1 , Jiang et al (2020) (hereafter Paper 2) studied the formation of isolated MSPs via NS-SS PT (a similar work is performed byNurmamat et al 2019). Paper 2 shows that, almost all the PT processes take place at the Roche Lobe overflow (RLOF) stage.…”