  In this work, we study the effect of strong magnetic fields on the equation
of state (EoS) of warm, homogeneous, Neutron Star (NS) matter in beta
equilibrium. NS matter is described within a relativistic mean field (RMF)
approximation, including both models with non-linear meson terms or with
density dependent nucleon-meson couplings. We first study the effect of
magnetic fields and finite temperature on the EoS separately, finding that the
effect of the latter to be significantly stronger than the one of the former.
We then study the combined effect of magnetic fields and temperature on the
internal composition. We show how both factors cause an increase in the proton
fraction at low density and that, as long as the temperatures considered are
not higher than 10 MeV, the effect of the magnetic field on the proton fraction
is not small enough to be neglected.
