Neutron star matter equation of state including <i>d</i><sup>*</sup>-hexaquark degrees of freedom
A. Mantziris, A. Pastore, I. Vidaña, D. P. Watts, M. Bashkanov, A. M. Romero
Abstract
We present the extension of a previous study where, assuming a simple free bosonic gas supplemented with a relativistic mean-field model to describe the pure nucleonic part of the equation of state, we studied the consequences that the first non-trivial hexaquark d * (2380) could have on the properties of neutron stars. Compared to that exploratory work, we employ a standard non-linear Walecka model including additional terms that describe the interaction of the d * (2380) di-baryon with the other particles of the system through the exchange of σ - and ω -meson fields. Our results show that the presence of the d * (2380) leads to maximum masses compatible with recent observations of ∼2 M ⊙ millisecond pulsars if the interaction of the d * (2380) is slightly repulsive or the d * (2380) does not interact at all. An attractive interaction makes the equation of state too soft to be able to support a 2 M ⊙ neutron star whereas an extremely repulsive one induces the collapse of the neutron star into a black hole as soon as the d * (2380) appears.