Abstract:
One of the intriguing mechanisms of the Sun is the formation of bipolar magnetic regions (BMRs) in the solar
convection zone (CZ), which are observed as regions of concentrated magnetic fields of opposite polarity on the
photosphere. These BMRs are tilted with respect to the equatorial line, which statistically increases with latitude.
The thin flux tube model, employing the rise of magnetically buoyant flux loops and their twist by Coriolis force, is
a popular paradigm for explaining the formation of tilted BMRs. In this study, we assess the validity of the thin flux
tube model by analysing the tracked BMR data obtained through the Automatic Tracking Algorithm for BMRs.
Our observations reveal that the tracked BMRs exhibit the expected collective behaviours. We find that the polarity
separation of BMRs increases over their normalized lifetime, supporting the assumption of a rising flux tube from
the CZ. Moreover, we observe an increasing trend of the tilt with the flux of the BMR, suggesting that rising flux
tubes associated with lower flux regions are primarily influenced by drag force and Coriolis force, while in higher
flux regions, magnetic buoyancy dominates. Furthermore, we observe Joy’s law dependence for emerging BMRs
from their first detection, indicating that at least a portion of the tilt observed in BMRs can be attributed to the
Coriolis force. Notably, lower flux regions exhibit a higher amount of fluctuations associated with their tilt
measurement compared to stronger flux regions, suggesting that lower flux regions are more susceptible to
turbulent convection.
