Sunspots or solar active regions are areas of concentrated magnetic fields on the solar surface that are formed as a result of the buoyant eruption of magnetic flux tubes from the interior of the Sun. The magnetic fields within these active regions are known to be twisted. The magnitude and distribution of the observed twist across the cross-section of the active region can give us important information about the dynamics of the underlying flux tube constituting the sunspot. This information, for example, can be related to how the flux tube interacted with the surrounding turbulent convection during its rise, or tell us about various instabilities (such as the kink-instability) that the flux tube may have been subject to; all these processes leave an imprint on the twist distribution in the active region magnetic fields. This project will involve an analysis of the observed twist distribution in solar active regions with the goal of understanding how this distribution relates to the afore-mentioned processes. Such a study is important for understanding the dynamics of magnetic flux tubes in stellar interiors and has implications for the subsequent flaring activity of twisted active regions.