Variation of Chromospheric Features as a Function of Latitude and Time Using Ca-K Spectroheliograms for Solar Cycles 15 – 23: Implications for Meridional Flow

We have analyzed the Ca-K images obtained at Kodaikanal Observatory as a function of latitude and time for period 1913 – 2004 covering Solar Cycles 15 to 23. classified chromospheric activity into plage, Enhanced Network (EN), Active (AN), Quiet (QN) areas differentiate between large strong active small weak regions. The regions represent toroidal poloidal component magnetic field. find that plage mostly up $50^{\circ }$ belt vary with about 11-year solar cycle. also represented by EN, AN QN varies significant amplitude $50^{\circ}$ in both hemispheres. variation is minimum around again increases amount polar region. In addition, plots plages, functions indicate maximum different occur epoch. To determine phase difference belts, we computed cross-correlation coefficients other belts $35^{\circ belt. shifts from mid-latitude towards equatorial high speed beginning cycle lower progresses. shift $\approx19$ $3~\text{m}\,\text{s}^{-1}$ considering all data observed period. This can be linked meridional flows, believed convection zone surface Sun.