  We report work towards a relativistic formulation for modeling strongly
magnetized neutron stars, rotating or in a close circular orbit around another
neutron star or black hole, under the approximations of helical symmetry and
ideal MHD. The quasi-stationary evolution is governed by the first law of
thermodynamics for helically symmetric systems, which is generalized to include
magnetic fields. The formulation involves an iterative scheme for solving the
Einstein-Maxwell and relativistic MHD-Euler equations numerically. The
resulting configurations for binary systems could be used as self-consistent
initial data for studying their inspiral and merger.
