Direct Observations of Plasma Upflows and Condensation in a Catastrophically Cooling Solar Transition Region Loop

TL;DR

This study presents direct observations of rapid plasma upflows and cooling in a solar transition region loop, linking magnetic reconnection to plasma dynamics and challenging existing solar atmospheric models.

Contribution

It provides the first detailed observational evidence connecting magnetic reconnection with fast transition region plasma upflows in cool solar loops.

Findings

Fast upflows ($v_ ext{lambda} \, \le \, -10$ km/s) observed at multiple TR temperatures.

Magnetic flux cancellation correlates with upflow regions.

Catastrophic cooling leads to plasma evaporation, indicating TR as the heating site.

Abstract

Minimal observational evidence exists for fast transition region (TR) upflows in the presence of cool loops. Observations of such occurrences challenge notions of standard solar atmospheric heating models, as well as their description of bright TR emission. Using the {\it EUV Imaging Spectrometer} (EIS) onboard {\it Hinode}, we observe fast upflows ($v_\lambda$\,$\le$\,$-$10 km s$^{-1}$) over multiple TR temperatures (5.8\,$\le$\,$\log T$\,$\le$ 6.0) at the footpoint sites of a cool loop ($\log T$\,$\le$\,6.0). Prior to cool loop energizing, asymmetric flows of $+$\,5 km s$^{-1}$ and $-$\,60 km s$^{-1}$ are observed at footpoint sites. These flows speeds and patterns occur simultaneously with both magnetic flux cancellation (at site of upflows only) derived from the {\it Solar Dynamics Observatory}'s (SDOs) { \it Helioseismic Magnetic Imager}'s (HMI) line-of-sight magnetogram images, and a 30\% mass in-flux at coronal heights. The incurred non-equilibrium structure of the cool loop leads to a catastrophic cooling event, with subsequent plasma evaporation indicating the TR as the heating site. From the magnetic flux evolution we conclude that magnetic reconnection between the footpoint and background field are responsible for observed fast TR plasma upflows.