“…The density dependence of the energy of the system and its pressure, as well as its compressibility, is analyzed for different proton fractions and magnetic fields. We will not consider β-equilibrium matter in most of the results shown, but will consider a wide range of nuclear matter asymmetries of interest for stellar matter, in particular, to the study of the inner crust, where a pasta phase is expected [49], to the study of matter with trapped neutrinos where large proton fractions are expected, which may be as large as 0.4 in the presence of a magnetic field [50], and to the study of neutrino free matter in β-equilibrium where the proton fraction will increase above 0.1 at subsaturation densities for a sufficiently strong magnetic field [51]. Therefore, besides symmetric nuclear matter and neutron matter, we choose two representative proton fractions, namely Y p = 0.1 for cold β-equilibrium matter and Y p = 0.3 for warm protoneutron star matter with a fraction of 0.4 trapped leptons.…”