06-175 Kiro Miyazaki
Neutron star moment-of-inertia in the extended Zimanyi-Moszkowski model (285K, PDF) Jun 2, 06
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Abstract. We revisit the extended Zimanyi-Moszkowski (EZM) model of dense neutron star (NS) core matter. In contrast to our previous work we treat the vector potentials of baryons on an equal footing with the effective masses, and solve a set of 6 equations to determine the three independent effective masses and vector potentials and a set of 2 equations to determine the conditions of beta-equilibrated NS matter, simultaneously. According to an expectation that the precisely measurable moment-of-inertia of J0737-3039A will impose a significant constraint on the nuclear equation-of-state (EOS), it is calculated using the two sets of hyperon coupling constants, EZM-SU6 and EZM-P, derived from the SU(6) symmetry and the empirical data of hypernuclei. We find I_{45}=1.23 and 1.64 that are close to the values in the EOSs of "APR" and "MS1" calculated by Morrison et al., while their mass-radius relations are rather different from the EZM models. The uniqueness of the EZM model is also apparent in the correlation map between the maximum gravitational mass of NS and the moment-of-inertia of J0737-3039A calculated for the other 25 EOSs by Bejger et al. Consequently, the EZM model is severely tested by the moment-of-inertia. However, whether the model is ruled out or not, there still remain some possibilities and problems of improving it.

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