Abstract
In the framework of the extended relativistic mean-field theory withhyperons, the properties of neutron star matter have beeninvestigated. It is found that at a density of four to five timesthat of nuclear matter saturation density ρ0, a neutron starwill become a hyperon star. This transition is strongly influenced bythe coupling constants of hyperons to mesons and a differentparameter set. For a given parameter set, a minimum transition baryondensity exists when the hyperon coupling ratios satisfyxHσ = xHω = xHρ = 0.65 orxHσ = xHω = 0.62, xHρ = 0.7.
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