  The purpose of this thesis is to obtain more realistic equations of state to
describe the matter forming magnetized white dwarfs, and use them to solve its
structure equations.
  The equations of state are determined by considering the weak magnetic field
approximation $B<B_c$ ($B_c=4.41\times10^{13}\text{ G}$) for the electron gas
of the star. The magnetic field introduces anisotropic pressures, even for the
moderate values present in white dwarfs. Also, we consider the energy and
pressure correction due to the Coulomb interaction of the electron gas with the
ions located in a crystal lattice.
  Moreover, spherically symmetric Tolman-Oppenheimer-Volkoff structure
equations are solved independently for the perpendicular and parallel
pressures, confirming the necessity of using axisymmetric structure equations,
more adequate to describe the anisotropic system. Therefore, we study the
solutions in cylindrical coordinates. In this case, the mass per longitude unit
is obtained instead of the total mass of the white dwarf.
