Super-Chandrasekhar White Dwarfs with Magnetic-dependent Equation of
  State
  Recently, some over-luminous Ia supernovaes are found, suggesting that their
progenitors are white dwarfs more massive than the Chandrasekhar limit, which
perhaps result from ultra-strong magnetic field inside the white dwarfs. We
present an equation of state, explicitly magnetic-dependent and analytically
practicable, and observe that the change of equation of states due to magnetic
field waning along radium will so significantly influence the configuration of
a white dwarf as that its density does not monotonically decrease, but goes
down at first, re-peaks near the crust and falls off again. As a supernovae
will, in the single degenerate Ia supernovae system, leave the remnant of its
companion and a neutron star (pulsar star), we point out that the observations
of these objects can put our model into tests
