Abstract
Abstract Coronal mass ejections are often considered to result from the full eruption of a magnetic flux rope (MFR). However, it is recognized that, in some events, the MFR may release only part of its flux, with the details of the implied splitting not completely established due to limitations in observations. Here, we investigate two partial eruption events including a confined and a successful one. Both partial eruptions are a consequence of the vertical splitting of a filament-hosting MFR involving internal reconnection. A loss of equilibrium in the rising part of the magnetic flux is suggested by the impulsive onset of both events and by the delayed onset of reconnection in the confined event. The remaining part of the flux might be line-tied to the photosphere in a bald patch (BP) separatrix surface, and we confirm the existence of extended BP sections for the successful eruption. The internal reconnection is signified by brightenings in the body of one filament and between the rising and remaining parts of both filaments. It evolves quickly into the standard current sheet reconnection in the wake of the eruption. As a result, regardless of being confined or successful, both eruptions produce hard X-ray sources and flare loops below the erupting but above the surviving flux, as well as a pair of flare ribbons enclosing the latter.
Highlights
Coronal mass ejections (CMEs) and solar flares are the most energetic explosions in the solar system
It is thought that the loss of equilibrium of an magnetic flux rope (MFR) leads to eruption (Forbes et al 2006; Chen 2011; Schmieder et al 2015)
Some of the brightened threads in the rising northwest part are seen to continue into the remaining southeast part with a common twisting pattern (Figure 1(c)–(d)). This suggests that the rising and remaining parts of the filament belong to the same MFR prior to the eruption, so that the reconnection associated with the vertical splitting is internal reconnection in agreement with the model by Gibson & Fan (2006b)
Summary
Coronal mass ejections (CMEs) and solar flares are the most energetic explosions in the solar system. Liu et al (2012) pointed out that a vertical split and subsequent partial eruption are possible in the much simpler configuration of an MFR above arcade-type flux, separated by an X-type magnetic structure referred to as a hyperbolic flux tube (HFT) In this case, the lower, surviving branch of the filament does not conform to the widespread assumption of a flux rope structure, but rather is contained in a magnetic arcade. The lower, surviving branch of the filament does not conform to the widespread assumption of a flux rope structure, but rather is contained in a magnetic arcade At present it is unclear which of the three suggested configurations— MFR with a BP or an HFT, or a double-decker MFR— represent the typical magnetic configuration prior to partial eruptions.
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