Evolution of a Coronal Twisted Flux Rope

TL;DR

This study uses multi-instrument solar observations to analyze the evolution of a twisted coronal flux rope associated with a flare and filament formation, providing insights into magnetic structure dynamics.

Contribution

It presents detailed observational evidence linking a twisted flux rope to filament formation and flare activity in the solar corona.

Findings

Detection of a twisted flux rope prior to filament formation

Correlation between flare brightening and flux rope evolution

Formation of an inverse S-shaped filament segment

Abstract

Multi-instrument observations of NOAA AR10938 on Jan. 14-18, 2007, are utilized to study the evolution of a magnetic thread system with multiple crossings suggestive of a twisted coronal flux rope. A C-class flare recorded by GOES on Jan. 16, at approximately 2:35 UT led to the brightening of the structure, that is seen in Hinode/EIS data at 2:46 UT, Hinode/XRT after 2:50 UT, and {\emph{STEREO}}/SECCHI/EUVI images at 3:30 UT. 304 {\AA} images revealed the presence of rapidly evolving, dark fibrils along the bright structure before and after the flare. A denser structure formed a few hours later and lasted for several days forming a segment of an inverse S-shaped filament. The present set of data is highly suggestive of the presence of a twisted flux rope prior to the formation of the filament segment at the same location.