Delta baryons in neutron stars

TL;DR

This paper investigates the impact of delta baryons and hyperons on neutron star properties using a relativistic mean-field model with density-dependent couplings, revealing conditions for delta-dominated stars and the effects on the equation of state.

Contribution

It introduces a detailed analysis of delta baryons in neutron stars with variable meson couplings, highlighting the possibility of delta-dominated stars and their influence on star properties.

Findings

Deltic stars with 80% delta baryons at the core are possible.

Hyperons reduce delta baryon fractions at high densities.

The equation of state stiffness is mainly influenced by omega-meson interactions.

Abstract

By applying a relativistic mean-field description of neutron star matter with density dependent couplings, we analyse the properties of two different matter compositions: nucleonic matter with delta baryons and nucleonic matter with hyperons and delta baryons. The delta-meson couplings are allowed to vary within a wide range of values obtained by experimental data, while the hyperon-meson couplings are fitted to hypernuclear properties. Neutron star properties with no deconfinement phase transition are studied. It is verified that many models are excluded because the effective nucleon mass becomes zero before the maximum mass configuration is attained. Hyperon-free with delta-dominated composition compact stars are possible, the deltic stars. It is found that with a convenient choice of parameters the existence of deltic stars with 80% of delta baryons at the center of the star is possible. However, the presence of hyperons lowers the delta baryon fraction to values below 20% at the center and below 30% at 2-3 saturation densities. It is discussed that in the presence of delta baryons, the hyperon softening is not so drastic because deltas couple more strongly to the $\omega$-meson, and the stiffness of the equation of state is determined by the $\omega$-dominance at high densities. The speed of sound reflects very well this behavior. The compactness of the pulsar RX J0720.4-3125 imposes $x_{\sigma\Delta}>x_{\omega\Delta}>1$ and favors $x_{\rho\Delta}>1$.