Role of vector channel in different classes of (non) magnetized neutron stars

TL;DR

This paper investigates how magnetic fields and vector channels influence the properties of various neutron star classes, comparing different models in hadronic and quark phases to understand their effects on star characteristics.

Contribution

It introduces the impact of non-standard vector channels and magnetic fields on neutron star models, comparing standard and extended frameworks in hadronic and quark phases.

Findings

Magnetic fields significantly affect star properties.

Inclusion of the $ ext{phi}$ meson alters hadronic star results.

Vector channels in quark models influence star stability.

Abstract

We study how the magnetic field and non-standard vector channels affect hadronic, quarkionic and hybrid stars. In the hadronic phase, we use the QHD model, within its standard $\sigma\omega\rho$ mesons, and compare the results with the ones obtained with the inclusion of the strangeness hidden $\phi$ meson. In the quark phase, we use the standard SU(3) NJL and compare the results with the version that takes into account the vector channel $G_v(\bar{\psi}\gamma^\mu\psi)$. Magnetic fields are taken into account via chaotic magnetic field approximation.