| Abstract : | Sunspots, seen as dark patches in the white light images of the Sun, are the regions of intense magnetic field on the surface of the Sun. These are essentially the poles of two opposite polarities of a more general feature, called the Bipolar Magnetic Regions (BMR), which can be observed in the full disk, Line of Sight (LOS) magnetograms. The decay and dispersal of BMR is responsible for producing the poloidal field in the Sun and thus plays a crucial role in the solar dynamo models. Hence, long-term study of various properties of BMR like the tilt, magnetic field strength, flux, are important for understanding the working of the solar dynamo. In our work, we are using the full disk LOS magnetogram data from space-borne instruments such as Michelson Doppler Imager (MDI; 1996–2011) with 96 minute cadence and Helioseismic and Magnetic Imager (HMI; 2010–2021) with 12 minute cadence. We use an automatic algorithm to identify and track BMRs for their lifetime or disk passage, starting from their first detection. Here, we present preliminary results of how the tilts, field strengths, and fluxes of the tracked BMRs vary over the course of their lifetimes. |
