研究太陽黑斑水平運動與觀測物理量之間的關係

Solar pores are small magnetic regions with concentrated and mostly verticalmagnetic fields. Their formation is closely related to the emergence anddissipation of magnetic flux. They are part of the earliest appearance of emergingflux at the photosphere and also the last remnant of decaying sunspots.Therefore, their observable characteristics can be used to verify models andsimulations of flux emergence, dissipation and evolution of sunspots. To date,magnetohydrodynamics modelling and simulations have been able to reproducemany aspectsof the structures, properties and evolution process of the pores. However, thehorizontal movements of the pores in many models or simulations are notcompletely consistent with the observed movements. This can indicate that someimportant physics and/or physical mechanisms have been omitted or incorrectlyimplemented in the models/simulations. Although the most advanced and realisticsimulations have produced motions qualitatively resembling the observations,there have been no comprehensive observational data for quantitativecomparison. The motivation and ultimate goal of this project is to investigatepossible physical mechanisms that drive the pores to move in a certain directionat any moment. The primary objective in the year of this current proposal is toinvestigate whether the movement is associated with any observable quantities.We plan to apply different statistical analysis techniques on large number ofpores to study the correlation and causality between the directions of motion andvariations of different observable quantities.