Estimation of the effect of hyperonic three-body forces on the maximum mass of neutron stars

Abstract

A model based on a microscopic Brueckner--Hartree--Fock approach of hyperonic matter supplemented with additional simple phenomenological density-dependent contact terms is employed to estimate the effect of hyperonic three-body forces on the maximum mass of neutron stars. Our results show that although hyperonic three-body forces can reconcile the maximum mass of hyperonic stars with the current limit of $1.4-1.5M_{\odot }$, they are unable to provide the repulsion needed to make the maximum mass compatible with the observation of massive neutron stars, such as the recent measurements of the unusually high masses of the millisecond pulsars PSR J1614-2230 ($1.97\pm 0.04M_{\odot }$) and PSR J1903+0327 ($1.667\pm 0.021M_{\odot }$).

6 pages, 1 figure, 2 tables. Accepted for publication in EPL

References in corpus (2)

• Shapiro delay measurement of a two solar mass neutron star
• An Eccentric Binary Millisecond Pulsar in the Galactic Plane

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