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Sunspots, identifiable as dark spots in white-light images, are regions with high concentrations of magnetic fields. In magnetograms, these sunspots appear as two adjacent regions with opposite magnetic polarities. Thus, in white-light images, sunspots represent the two poles of a larger structure called bipolar magnetic regions (BMRs). Typically, sunspots exhibit a tilt relative to the solar equator, known as the tilt angle. The tilt angles of these BMRs or sunspots are vital for understanding solar-dynamo models.
The Kodaikanal Solar Observatory (KSO) has an extensive history of capturing solar observations across three different wavelengths: white light, Ca-II K, and H-alpha. For this study, we have focused on the white-light data from KSO. Employing a semi-automatic method, we identified sunspot groups and calculated their tilt angles for the period from 1954 to 1964 (one solar cycle). These tilt angles will help us verifying the joys law and such things.
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