The importance of strange mesons in neutron star properties

Abstract

In order to obtain the properties of compact stellar objects, appropriate equations of state have to be used. In the literature, strange meson fields, namely the scalar meson field σ * (975) and the vector meson field φ(1020), had to be considered in order to reproduce the observed strongly attractive ΛΛ interaction. The introduction of these strange mesons makes the equations of state harder (EOS) due to the repulsive effect of the φ(1020) meson. In this work the inclusion of these mesons in the equation of state and their influence on the properties of the neutron stars are investigated.

Hyperonic neutron stars: reconciliation between nuclear properties and NICER and LIGO/VIRGO results

“…as pointed in ref. [12,[18][19][20], this vector channel is crucial to obtain massive hyperonic neutron stars. The second one is a non-linear ω-ρ coupling meson as present in the IUFSU model [15]:…”

Hypermassive quark cores

“…as pointed out in ref. [14,[20][21][22], this vector channel is crucial to obtain massive hyperonic neutron stars. The second one is a non-linear ω-ρ coupling term [23]:…”

The neutron star inner crust: an empirical essay

“…At such densities new and exotic degrees of freedom can be present. The most common non-nucleonic degrees of freedom studied in the literature are the hyperons [24,38,[40][41][42][43]. Another possibilities are the onset of ∆ ′ s resonance and boson condensation [38,44].…”