Abstract

Observations of polar faculae and magnetic fields have shown that solar activity at high heliospheric latitude presents an important part of the solar cycle. Detection of strong (B > 1000G) magnetic fields in small areas of polar faculae (Homann et al.,1997) shows that we should not expect very different nature and structure in polar zones as compared with ones at low latitudes. More over there is connection between fluctuations of the polar activity and sunspot numbers in the following solar cycle. Today we have a number of new methods to register the polar activity: EUV observations from SOHO, high = sensitivity and spartial resolution magnetograms. The Nobeyama radioheliograph working since 1992 at wavelength of 1.76 cm presents an unprecedented set of regular observations of the Sun. We compared polar faculae found from white-light observtions at the Kislovodsk Solar Station, polar magnetic knots at the Kitt Peak magnetograms, bright points on the EIT SOHO with ones from Nobeyama radioheliograph for a few selected dates. A physical model of the 3D-structure of magnetosphere of polar faculae is discussed.