Strange quark stars in binaries: formation rates, mergers and explosive phenomena

TL;DR

This paper models the formation and population of strange quark stars in binary systems, exploring their potential for explosive phenomena and their observational signatures, based on a two-families scenario and population synthesis.

Contribution

It introduces a large-scale population synthesis model incorporating the two-families scenario to study the distribution and formation of strange quark stars in binaries.

Findings

Strange quark stars form mainly via accretion onto neutron stars.

The mass range for coexistence of neutron and strange quark stars is identified.

Merger rates of strange quark star systems are very low, consistent with experimental limits.

Abstract

The existence of strange quark stars has been proposed many years ago. More recently, the possible co-existence of a first family composed of "normal" neutron stars with a second family of strange quark stars has been proposed as a solution of problems related to the maximum mass and to the minimal radius of these compact stellar objects. In this paper we study the mass distribution of compact objects formed in binary systems and the relative fractions of quark and neutron stars in different subpopulations. We incorporate the strange quark star formation model provided by the two-families scenario and we perform a large-scale population synthesis study in order to obtain the population characteristics. In our model, below a critical gravitational mass $M_\mathrm{max}^H- \Delta M$ only normal (hadron) neutron stars exist. Then in the mass range $(M_\mathrm{max}^H- \Delta M) \leqslant M \leqslant M_\mathrm{max}^H$ strange quark stars and neutron stars coexist. Finally, above $M_\mathrm{max}^H$ all compact objects are strange quark stars. We argue that $M_\mathrm{max}^H$ is in the range $\sim 1.5-1.6 M_\odot$. According to our results, the main channel for strange quark star formation in binary systems is accretion from a secondary companion on a neutron star.This opens the possibility of having explosive GRB-like phenomena not related to supernovae and not due to the merger of two neutron stars. The enhancement in the number of compact objects in the co-existence mass range $(M_\mathrm{max}^H- \Delta M) \leqslant M \leqslant M_\mathrm{max}^H$ is not very pronounced. The number of double strange quark star's systems is rather small with only a tiny fraction which merge within a Hubble time. This drastically limits the flux of strangelets produced by the merger, which turns out to be compatible with all limits stemming from Earth and lunar experiments.