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We present an analysis of the formation of atmospheric flux ropes in amagnetohydrodynamic (MHD) solar flux emergence simulation. The simulationdomain ranges from the top of the solar interior to the low corona. A twistedmagnetic flux tube emerges from the solar interior and into the atmospherewhere it interacts with the ambient magnetic field. By studying theconnectivity of the evolving magnetic field, we are able to better understandthe process of flux rope formation in the solar atmosphere. In the simulation,two flux ropes are produced as a result of flux emergence. Each has a differentevolution resulting in different topological structures. These are determinedby plasma flows and magnetic reconnection. As the flux rope is the basicstructure of the coronal mass ejection (CME), we discuss the implications ofour findings for solar eruptions.

On magnetic reconnection and flux rope topology in solar flux emergence