The Role of Magnetic Reconnection in the Observable Features of Solar Eruptions

144 citations recorded by the source corpus.

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

Direct Observations of the Magnetic Reconnection Site of an Eruption on 2003 November 18 (2005, background): “It appears to show the shape of a flux rope surrounded by a bubble (see, e.g., Lin et al. 2004).”
On the Magnetic Flux Budget in Low-Corona Magnetic Reconnection and Interplanetary Coronal Mass Ejections (2007, background): “…in both of these scenarios may maintain stability for a relatively long timescale prior to the explosive loss of equilibrium (Forbes & Priest 1995; Lin et al. 2004) or a breakout type reconnection that opens up the overlying flux of opposite polarities (Antiochos et al. 1999; Lynch et al. 2004).”
DIRECT EVIDENCE FOR A FAST CORONAL MASS EJECTION DRIVEN BY THE PRIOR FORMATION AND SUBSEQUENT DESTABILIZATION OF A MAGNETIC FLUX ROPE (2012, methodology): “These patterns are compatible with magnetic reconnection during the confined flare adding new magnetic flux to the flux rope (e.g., Lin et al. 2004).”
The CME-flare relationship: Are there really two types of CMEs? (2005, background): “Firstly, the reconnection reduces the net tension of the overlaying arcade field and increases the magnetic pressure below the erupting flux-rope (e.g., Van Tend & Kuperus 1978; Anzer & Pneuman 1982; Forbes 1990; Cheng et al. 2003; Lin et al. 2004).”