Context : We introduced the technique of model atmosphere calculation with polarized radiative transfer and magnetic line blanketing .
However , the calculation of model atmospheres with realistic magnetic field configurations ( field strength and angle defined relative to the atmosphere plane ) has not been previously attempted .

Aims : In the last paper of this series we study the effects of the magnetic field , varying its strength and orientation , on the model atmosphere structure , the energy distribution , photometric colors and the hydrogen Balmer line profiles .
We compare with the previous results for an isotropic case in order to understand whether there is a clear relation between the value of the magnetic field angle and model changes , and to study how important the additional orientational information is .
Also , we examine the probable explanation of the visual flux depressions of the magnetic chemically peculiar stars in the context of this work .

Methods : We calculated one more grid of the model atmospheres of magnetic A and B stars for different effective temperatures ( { T _ { eff } = 8000 } K , 11 000 K , 15 000 K ) , magnetic field strengths ( { B = 0 } , 5 , 10 , 40 kG ) and various angles of the magnetic field ( { \Omega = 0 \degr } – 90 \degr ) with respect to the atmosphere plane .
We used the LLModels code which implements a direct method for line opacity calculation , anomalous Zeeman splitting of spectral lines , and polarized radiation transfer .

Results : We have not found significant changes in model atmosphere structure , photometric and spectroscopic observables or profiles of hydrogen Balmer lines as we vary the magnetic field inclination angle \Omega .
The strength of the magnetic field plays the main role in magnetic line blanketing .
We show that the magnetic field has a clear relation to the visual flux depressions of the magnetic CP stars .

Conclusions : We can use the approach introduced in the previous paper of this series , which neglects anisotropy effects , to calculate model atmospheres with magnetic line blanketing .
This technique seems to be reliable , at least for homogeneous atmospheres with scaled solar abundances .