Tracking moving magnetic features in the photosphere

Abstract

sun, activity, magnetic fields, photosphere, sunspots, moat, moving magnetic features On magnetograms, small-scale Moving Magnetic Features (MMFs) of both the same and opposite to the sunspots' magnetic field are observed to originate near the penumbra boundary and stream almost radially outward within the moat at a speed about 1 km/s and finally disappear in the moat or merge into the surrounding network. This flux outflow plays an intricate role in the mass and magnetic energy flow around sunspots and contributes to the evolution of the sunspots. MMFs can be bipolar or unipolar. Observing MMFs requires consecutive, short time-cadence, and high

Recent progress in solar physics made during the program of 2008 August 1st solar total eclipse

“…Tracking moving magnetic features (MMF) in the photosphere is an important approach to monitoring and forecasting solar activities and possible eruptions. Li et al [3] developed a code for tracking the MMF in the observational data automatically, and used this code to track MMFs around 26 sunspots. These MMFs were found to travel on average 3.8×10 3 km at speed around 0.6 km/s.…”