Low-mass X-ray Binaries with Strange Quark Stars

Abstract

Strange quark stars (SSs) may originate from accreting neutron stars (NSs) in low-mass X-ray binaries (LMXBs). Assuming that conversion of NS matter to SSs occurs when the core density of accreting NS reaches to the density of quark deconfinement, $\sim 5{\rho }_0$, where ${\rho }_0\sim 2.7\times 10^{14}$g cm${}^{-3}$ is nuclear saturation density, we investigate LMXBs with SSs (qLMXBs). In our simulations, about 1\permil --- 10% of LMXBs can produce SSs, which greatly depends on the masses of nascent NSs and the fraction of transferred matter accreted by the NSs. If the conversion does not affect binaries systems, LMXBs evolve into qLMXBs. We find that some observational properties (spin periods, X-ray luminosities and orbital periods) of qLMXBs are similar with those of LMXBs, and it is difficult to differ them. If the conversion disturbs the binaries systems, LMXBs can produce isolated SSs. These isolated SSs could be submillisecond pulsars, and their birthrate in the Galaxy is $\sim$5--70 per Myr.

6 pages, 6 figures

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• A strange star scenario for the formation of isolated millisecond pulsars
• Heavy element contributions of rotating massive stars to Interstellar Medium
• A Strange Star Scenario for the Formation of Eccentric Millisecond Pulsar PSR J1946+3417
• Optical Properties of C$-$rich (${}^{12}$C, SiC and FeC) Dust Layered Structure of Massive Stars
• Quark Novae: An Alternative Channel For the Formation of Isolated Millisecond Pulsars