SOLARNET Conference: The Many Scales of the Magnetic Sun

Solar pores are associated with the concetration, dissipation, and transportation of solar magnetic fluxes. Their observable characteristics can provide important constraints to improve models and simulations of magnetic flux emergence and formation. In this work, we have investigated the horizontal movements of solar pores. The goal is to probe possible correlations of observable quantities with the movement of the pore. Our statistical analysis on 61 compact pores identified from the Spaceweather HMI Active Region Patches from 2011 to 2018 shows that the direction of movement is either parallel or anti-parallel to the direction of maximum magnetic pressure difference at the opposite sides of the edges of the pores. The correlation coefficients for both parallel and anti-parallel cases are both higher than 0.74. Despite having a high correlation, our information theoretic analysis using transfer entropy indicates no significant causal relationship between the direction of motion and the direction of maximum magnetic pressure difference.