  We systematically study the properties of pure nucleonic and hyperonic
magnetic stars using a density-dependent relativistic mean field (DD-RMF)
equations of state. We explore several parameter sets and hyperon coupling
schemes within the DD-RMF formalism. We focus on sets that are in better
agreement with nuclear and other astrophysical data, while generating heavy
neutron stars. Magnetic field effects are included in the matter equation of
state and in general relativity solutions, which in addition fulfill Maxwell's
equations. We find that pure nucleonic matter, even without magnetic field
effects, generates neutron stars that satisfy the potential GW190814 mass
constraint; however, this is not the case for hyperonic matter, which instead
only satisfies the more conservative 2.1 M$_{\odot}$ constraint. In the
presence of strong but still somehow realistic internal magnetic fields
$\approx10^{17}$ G, the stellar charged particle population re-leptonizes and
de-hyperonizes. As a consequence, magnetic fields stiffen hyperonic equations
of state and generate more massive neutron stars, which can satisfy the
possible GW190814 mass constraint but present a large deformation with respect
to spherical symmetry.
