The properties of neutron star in its evolution

In the relativistic σ-ω model, the equation of states of npeμ neutron star matter and strange-star matter which include various strange particles are discussed, respectively. Since the maximum mass of the npeμ neutron star ( 2.01M O .) is larger than the one of the strange star ( 1.4M O .), and the mass of the neutron star accretes in its evolution, we predict that the strange particles are abundant on the birth of the neutron star, corresponding to the radio pulsar and X-ray pulsar; the abundance of strange particles decreases as the neutron star evolutes, and the strange star becomes the npeμ neutron star in the end of the evolution, corresponding to the neutron stars in low-mass X-ray binaries (LMXBs).