  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.
