Аннотация:The interconnection between Saturn's polar regions is studied, with the main attention being paid to the influence of the interplanetary magnetic field (IMF)on this process. The most complex case arises for southward IMF. For an example event in February 2008 (DOY 43) when we have both the UV image of the southern polar region obtained by the Hubble Space Telescope and the IMF at the nose of the kronian magnetosphere measured by Cassini, we
calculate the field-aligned projections of the bright emissions in the southern polar region to the magnetospheric equatorial plane and to the northern Saturn's hemisphere. For this purpose we use our paraboloid magnetospheric model which has newly been modified by taking into account the multipole terms of the internal planetary magnetic field and the
spheroidal form of the planet’s conducting ionosphere. Our results show that there should be
rather similar patterns of bright spots in both polar caps. However, the whole magnetic field structure and consequently the character of the emission in the high latitude ionosphere depend on the IMF component along the planetary dipole direction.