We demonstrate the subsurface origin of the observed evolution of the solar active region 10930 (AR10930) associated with merging and breakup of magnetic polarity regions at the solar surface. We performed a magnetohydrodynamic simulation of an emerging magnetic flux tube whose field-line twist is asymmetrically distributed along its axis, which is a key to merging and fragmentation in this active region. While emerging into the surface, the flux tube is subjected to partial splitting of its weakly twisted portion, forming separate polarity regions at the solar surface. As emergence proceeds, these separate polarity regions start to merge and then break up, while in the corona sigmoidal structures form and a solar eruption occurs. We discuss what physical processes could be involved in the characteristic evolution of an active region magnetic field that leads to the formation of a sunspot surrounded by satellite polarity regions.

Abstract
1. INTRODUCTION
2. MODEL DESCRIPTION
3. RESULTS
    3.1. Surface Evolution
    3.2. Coronal Evolution
4. DISCUSSION
REFERENCES

• Tetsuya Magara(Department of Astronomy and Space Science, Kyung Hee University/School of Space Research, Kyung Hee University) Corresponding author