Multi-Viewpoint Observation of a Failed Prominence Eruption on the Sun

TL;DR

This study provides a detailed multi-viewpoint observation of a failed solar prominence eruption, revealing the roles of different magnetic reconnection processes in eruption dynamics.

Contribution

It offers new insights into the mechanisms of solar eruptions by analyzing the interplay of reconnection processes during a failure event.

Findings

External reconnection occurs on the erupting flux rope.

The flux rope's acceleration is influenced by reconnection processes.

Failed eruption results from magnetic confinement by overlying fields.

Abstract

Solar eruptions are sudden ejections of coronal mass and magnetic fields accompanied by intense energy release. The eruptive structure does not always erupt successfully, but sometimes fails to escape the Sun after initiation. The failure of an eruption, however, provides an invaluable opportunity for understanding the intricate mechanism of eruptions. We present a comprehensive observation of a failed prominence eruption on the Sun, taking advantage of multi-viewpoint and multi-messenger imaging. Simultaneous off-limb and on-disk observation gives evidence of magnetic reconnection processes occurring at different sites during the flare. Particularly, in addition to the standard flare reconnection behind the eruption, strong external reconnection occurs on the erupting flux rope, evidenced by a wealth of signatures via multi-wavelength imaging and spectroscopy. The two reconnection processes may play contrasting roles in the flux rope's acceleration and compete in altering the magnetic flux in the rope. As the high rate of external reconnection proceeds, the flux rope and embedded prominence decelerate noticeably and fail to erupt into the heliosphere, under strong magnetic confinement of overlying fields. Our results illustrate a well-defined physical picture for solar eruptive activities and provide insight into the lack of coronal mass ejections found in other solar-type stars.