  In this paper a theoretical model of a magnetic white dwarf is studied. All
numerical calculations are performed under the assumption of a spherically
symmetric star. The obtained equation of state is stiffer for the increasing
value of magnetic field B. The numerical values of the maximum mass and radius
are presented. Sensibility of the results to the choice of the magnetic field
strength is evident. Finally the departure from the condition of isothermality
of degenerated electron gas in gravitational field is discussed.
