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By relating scalar and vector couplings of the hyperons to the inferred empirical binding of the hyperon in saturated nuclear matter, we obtain compatibility of this binding energy with neutron-star masses. Use of the observational constraint on the lower bound on the maximum neutron-star mass and the upper bound of the couplings that are compatible with hypernuclear levels, places bounds on the reduction in neutron-star mass that hyperons produce. For the best current estimate of nuclear-matter properties, the reduction in mass due to conversion of nucleons to hyperons is (0. 710. 15) M_. Neutrons comprise a slight majority population M_ neutron stars with mass 1. 5M_.
Glendenning et al. (Tue,) studied this question.