Evidence for Hot Fast Flow above a Solar Flare Aracade

TL;DR

This study provides spectroscopic evidence of hot, fast plasma flows above a solar flare loop, supporting the magnetic reconnection model of flare energy release.

Contribution

First spectroscopic scanning observation confirming the presence of hot fast flows above a flare loop, validating key aspects of the standard eruptive flare model.

Findings

Hot (~30MK) fast (>500 km/s) plasma flows located above the flare loop.

Supports the magnetic reconnection model occurring above the flare loop.

Provides quantitative two-dimensional structure measurement of hot fast flows.

Abstract

Solar flares are one of the main forces behind space weather events. However the mechanism that drives such energetic phenomena is not fully understood. The standard eruptive flare model predicts that magnetic reconnection occurs high in the corona where hot fast flows are created. Some imaging or spectroscopic observations have indicated the presence of these hot fast flows but there have been no spectroscopic scanning observation to date to measure the two-dimensional structure quantitatively. We analyzed a flare that occurred on the west solar limb on 27 January 2012 observed by the Hinode EUV Imaging Spectrometer (EIS) and found that the hot (~30MK) fast (>500 km/s) component was located above the flare loop. This is consistent with magnetic reconnection taking place above the flare loop.