A numerical model is used to study systematically the evolution of large scale irregularities depending on the IMF Bz and By components, solar zenith angle (seasonal and daily variation), solar and geomagnetic activity. The model enables to reproduce the 3-D distribution of electron density over the high-latitude F region ionosphere in the altitude range between 130 and 640 km. Since the convection electric field driven by changes in solar wind conditions has an important effect on the high-latitude ionosphere, the rotation of the IMF vector in the Y–Z plane causes a significant redistribution of the ionospheric plasma. Under the southward IMF conditions the plasma density is enhanced over a large portion of the near-pole ionosphere as a tongue of ionization, while the northward IMF leads to a considerable depletion and occurrence of the polar hole. The IMF By polarity is crucial for the shift and extension of the tongue of ionization to the dusk or dawn side. Particle precipitation also plays a role through a localized increase of the electron density mostly within the auroral oval and more pronounced auroral peak. The solar zenith angle, especially its seasonal variation, is the strongest regular factor influencing the electron density magnitude and spatial distribution. In winter, when the polar ionosphere is in darkness, large variations associated with different solar wind condition are more prominent. The daily variation of the zenith angle considerably modifies the Ne within a particular pattern. At a given time, the combined action of the IMF, solar zenith angle, level of solar and geomagnetic activity produces a complicated ionospheric response which can be considered as a superposition of different effects. Quantitative estimates of the ionospheric response to each factor are presented.