Break up of returning plasma after the 7 June 2011 filament eruption by Rayleigh-Taylor instabilities

TL;DR

This paper analyzes the plasma structures resulting from the 2011 solar filament eruption, focusing on Rayleigh-Taylor instabilities and their role in the breakup of falling plasma, using SDO/AIA imaging data.

Contribution

It identifies and examines Rayleigh-Taylor instabilities in solar plasma falling after a filament eruption, estimating Alfven velocities and describing new self-similar branching features.

Findings

Rayleigh-Taylor instabilities observed in falling plasma

Estimated Alfven velocities from instability features

Identified self-similar branching horn structures

Abstract

A prominence eruption on 7 June 2011 produced spectacular curtains of plasma falling through the lower corona. At the solar surface they created an incredible display of extreme ultraviolet brightenings. The aim is to identify and analyze some of the local instabilities which produce structure in the falling plasma. The structures were investigated using SDO/AIA 171A and 193A images in which the falling plasma appeared dark against the bright coronal emission. Several instances of the Rayleigh-Taylor instability were investigated. In two cases the Alfven velocity associated with the dense plasma could be estimated from the separation of the Rayleigh-Taylor fingers. A second type of feature, which has the appearance of self-similar branching horns, is also discussed.