Hyperonic uncertainties in neutron stars, mergers and supernovae

TL;DR

This paper investigates how uncertainties in hyperonic interactions affect the equation of state and observable properties of neutron stars, mergers, and supernovae, especially at high temperatures, using extended hadronic models.

Contribution

It introduces new hyperonic models that encompass the full range of experimental uncertainties and analyzes their impact on astrophysical phenomena.

Findings

Hyperonic uncertainties influence particle abundances and the EoS.

Effects are more significant at higher temperatures.

Implications for neutron star merger and supernova simulations.

Abstract

In this work we delve into the temperature-dependent Equation of State (EoS) of baryonic matter within the framework of the FSU2H$^*$ hadronic model, which comprehensively incorporates hyperons and is suitable for relativistic simulations of neutron star mergers and supernovae. To assess the impact of the uncertainties in the hyperonic sector on astrophysical observables, we introduce two additional models, namely FSU2H$^*$L and FSU2H$^*$U. These models cover the entire spectrum of variability of hyperonic potentials, as derived from experimental data. Our investigations reveal that these uncertainties extend their influence not only to the relative abundances of various particle species but also to the EoS itself and, consequently, have an impact on the global properties of both cold and hot neutron stars. Notably, their effects become more pronounced at large temperatures, owing to the increased presence of hyperons. These findings have direct implications for the outcomes of relativistic simulations of neutron star mergers and supernovae, emphasizing the need of accounting for hyperonic uncertainties to ensure the accuracy and reliability of such simulations in astrophysical contexts.