Role of vector channel in different classes of (non) magnetized neutron stars
We study how the magnetic field and non-standard vector channels affect hadronic, quark and hybrid stars. In the hadronic phase, we use the QHD model, with its standard $$\sigma \omega \rho $$ σ ω ρ mesons, and compare the results with the ones obtained with the inclusion of the strangeness hidden $$\phi $$ ϕ 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 $$G_v({\bar{\psi }}\gamma ^\mu \psi )$$ G v ( ψ ¯ γ μ ψ ) . Magnetic fields are taken into account via chaotic magnetic field approximation.