  The technique of model atmosphere calculation for magnetic Ap and Bp stars
with polarized radiative transfer and magnetic line blanketing is presented. A
grid of model atmospheres of A and B stars are computed. These calculations are
based on direct treatment of the opacities due to the bound-bound transitions
that ensures an accurate and detailed description of the line absorption and
anomalous Zeeman splitting. The set of model atmospheres was calculated for the
field strengths between 1 and 40 kG. The high-resolution energy distribution,
photometric colors and the hydrogen Balmer line profiles are computed for
magnetic stars with different metallicities and are compared to those of
non-magnetic reference models and to the previous paper of this series. The
results of modelling confirmed the main outcomes of the previous study: energy
redistribution from UV to the visual region and flux depression at 5200A.
However, we found that effects of enhanced line blanketing when transfer for
polarized radiation takes place are smaller in comparison to those obtained in
our first paper where polarized radiative transfer was neglected. Also we found
that the peculiar photometric parameter delta_a is not able to clearly
distinguish stellar atmospheres with abundances other than solar, and is less
sensitive than delta(V_1-G) or Z to a magnetic field for low effective
temperature (Teff=8000K). Moreover we found that the back determination of the
fundamental stellar atmosphere parameters using synthetic Stromgren photometry
does not result in significant errors.
