Many-body forces in the equation of state of hyperonic matter

Abstract

In this work we introduce an extended version of the formalism proposed originally by Taurines et al. that considers the effects of many-body forces simulated by non-linear self-couplings and meson-meson interaction contributions. In this extended version of the model, we assume that matter is at zero temperature, charge neutral and in beta-equilibrium, considering that the baryon octet interacts by the exchange of scalar-isoscalar ($\sigma$,${\sigma }^{\ast }$), vector-isoscalar ($\omega$,$\varphi$), vector-isovector ($\varrho$) and scalar-isovector ($\delta$) meson fields. Using nuclear matter properties, we constrain the parameters of the model that describe the intensity of the indirectly density dependent baryon-meson couplings to a small range of possible values. We then investigate asymmetric hyperonic matter properties. We report that the formalism developed in this work is in agreement with experimental data and also allows for the existence of massive hyperon stars (with more than $2M_{\odot }$) with small radii, compatible with astrophysical observations.

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• Chiral symmetry restoration and the $\Delta$ matter formation in neutron stars
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• The dissipation of toroidal magnetic fields and spin-down evolution of young and strongly magnetized pulsars
• Equation of state and composition of proto-neutron stars and merger remnants with hyperons
• Revisiting the Equation of State of Hybrid Stars in the Dyson-Schwinger Equation Approach to QCD
• The Role of Baryon Structure in Neutron Stars
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• Massive relativistic compact stars from SU(3) symmetric quark models
• The Magnetic Field Distribution in Strongly Magnetized Neutron Stars
• Influence of the nuclear symmetry energy slope on observables of compact stars with $\Delta$-admixed hypernuclear matter
• Fundamental Oscillation Modes in Neutron Stars with Hyperons and Delta Baryons
• Many-body forces, isospin asymmetry and dense hyperonic matter