English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Solar flare termination shocks have been suggested as one of the viablemechanisms for accelerating electrons and ions to high energies. Observationalevidence of such shocks, however, remains rare. Using radio dynamicspectroscopic imaging of a long-duration C1.9 flare obtained by the Karl G.Jansky Very Large Array (VLA), Chen et al. (2015) suggested that a type ofcoherent radio bursts, referred to as "stochastic spike bursts," were radiosignatures of nonthermal electrons interacting with myriad density fluctuationsat the front of a flare termination shock. Here we report another stochasticspike burst event recorded during the extended energy release phase of along-duration M8.4-class eruptive flare on 2012 March 10. VLA radiospectroscopic imaging of the spikes in 1.0--1.6 GHz shows that similar to thecase of Chen et al. (2015), the burst centroids form an extended, ~10''-longstructure in the corona. By combining extreme-ultraviolet imaging observationsof the flare from two vantage points with hard X-ray and ultravioletobservations of the flare ribbon brightenings, we reconstruct the flare arcadein three dimensions. The results show that the spike source is located at ~60Mm above the flare arcade, where a diffuse supra-arcade fan and multitudes ofplasma downflows are present. Although the flare arcade and ribbons seen duringthe impulsive phase do not allow us to clearly understand how the observedspike source location is connected to the flare geometry, the cooling flarearcade observed two hours later suggests that the spikes are located in theabove-the-loop-top region, where a termination shock presumably forms.

Radio Spectral Imaging of an M8.4 Eruptive Solar Flare: Possible Evidence of a Termination Shock