Formation of twin compact stars in low-mass X-ray binaries: Implications on eccentric and isolated millisecond pulsar populations

TL;DR

This paper explores how rapid phase transitions in neutron stars within low-mass X-ray binaries can lead to the formation of twin compact stars and influence the orbital characteristics of millisecond pulsars, offering insights into dense matter physics.

Contribution

It demonstrates that accretion-induced phase transitions can produce observable effects on MSP orbits and provides a model linking stellar evolution with dense matter properties.

Findings

Phase transitions can occur during the LMXB phase or spin-down phase.

Eccentric binary MSPs may form from systems with wider orbits.

Orbital eccentricity distribution can constrain phase transition models.

Abstract

Millisecond pulsars (MSPs) are laboratories for stellar evolution, strong gravity, and ultra-dense matter. Although MSPs are thought to originate in low-mass X-ray binaries (LMXBs), approximately 27% lack a binary companion, and others are found in systems with large orbital eccentricities. Understanding how these systems form may provide insight into the internal properties of neutron stars (NSs). We studied the formation of a twin compact star through rapid first-order phase transitions in NS cores due to mass accretion in LMXBs. We investigated whether this mechanism, possibly coupled with secondary kick effects such as neutrino or electromagnetic rocket effects, leaves an observable long-lasting imprint on the orbit. We simulated mass accretion in LMXBs consisting of a NS and a low-mass main-sequence companion and followed the evolution of the NS mass, radius, and spin until a strong phase transition is triggered. For the NS structure, we assumed a multi-polytrope equation of state that allows for a sharp phase transition from hadronic to quark matter and satisfies observational constraints. We find that in compact binaries with relatively short pre-Roche lobe overflow orbital periods, an accretion-induced phase transition can occur during the LMXB phase. In contrast, in systems with wider orbits, this transition can take place during the spin-down phase, forming an eccentric binary MSP. If the transition is accompanied by a secondary kick, then the binary is likely to be disrupted, forming an isolated MSP or re-configured into an ultra-wide orbit. Our findings suggest that accretion in LMXBs provides a viable path for forming twin compact stars, potentially leaving an observable imprint on the orbit. The eccentricity distribution of binary MSPs with long orbital periods (> 50 d) could provide constraints on first-order phase transitions in dense nuclear matter.