Abstract. Previous studies show that there is a lack of information on the variation of network flux with solar cycle phase and also the center of solar disc was found to show no variation with solar cycle phase (White \& Livingston, 1978, ApJ, 226, 679). A study on solar variability model (Skumanich et al. 1984, ApJ, 282, 776) shows that there is an excess component during the solar maximum phase. So the above mentioned studies, forms the basis for the development of new programme (Jagdev Singh 1989) at Kodaikanal tower telescope in 1986 to monitor Ca K line profiles as a function of latitude and integrated over the visible 180^o longitude. The observations have been taken from 1986 onwards. Thus the huge database will be used to study the various parameters of the Ca K line and to study the variation of network flux as a function of solar latitude with solar cycle phase. Activity related with sunspots has been studied widely but variations in the polar regions have not been observed systematically. Our data permits to study the changes in polar regions systematically and its implications to the magnetic cycle of the Sun. So the observations, methods, data analysis procedures, preliminary results will be discussed.