Observational Evidence of Sausage-Pinch Instability in Solar Corona by SDO/AIA

TL;DR

This paper provides the first observational evidence of sausage-pinch instability in the solar corona, showing how magnetic flux tubes evolve and stabilize during a prominence eruption using SDO/AIA data.

Contribution

It presents direct observational evidence of sausage-pinch instability in a solar flux tube, highlighting its morphological signatures and dynamic behavior during an eruption.

Findings

Identification of flux tube curvatures with variable cross-sections

Observation of bright knots and narrow regions indicating instability

Detection of plasma flows along magnetic field lines that influence stability

Abstract

We present the first observational evidence of the evolution of sausage-pinch instability in Active Region 11295 during a prominence eruption using data recorded on 12 September 2011 by the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO). We have identified a magnetic flux tube visible in AIA 304 \AA\ that shows curvatures on its surface with variable cross-sections as well as enhanced brightness. These curvatures evolved and thereafter smoothed out within a time-scale of a minute. The curved locations on the flux tube exhibit a radial outward enhancement of the surface of about 1-2 Mm (factor of 2 larger than the original thickness of the flux tube) from the equilibrium position. AIA 193 \AA\ snapshots also show the formation of bright knots and narrow regions inbetween at the four locations as that of 304 \AA\ along the flux tube where plasma emission is larger compared to the background. The formation of bright knots over an entire flux tube as well as the narrow regions in < 60 s may be the morphological signature of the sausage instability. We also find the flows of the confined plasma in these bright knots along the field lines, which indicates the dynamicity of the flux tube that probably causes the dominance of the longitudinal field component over short temporal scales. The observed longitudinal motion of the plasma frozen in the magnetic field lines further vanishes the formed curvatures and plasma confinements as well as growth of instability to stablize the flux tube.