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

We have investigated an M1.3 limb flare, which develops as a magneticloop/arch that fans out from an X-ray jet. Using Hinode/EIS, we found that thetemperature increases with height to a value of over 10$^{7}$ K at the loop-topduring the flare. The measured Doppler velocity (redshifts of 100$-$500 kms$^{-1}$) and the non-thermal velocity ($\geq$100 km s$^{-1}$) from Fe XXIValso increase with loop height. The electron density increases from$0.3\times10^{9}$ cm$^{-3}$ early in the flare rise to $1.3\times10^{9}$cm$^{-3}$ after the flare peak. The 3-D structure of the loop derived withSTEREO/EUVI indicates that the strong redshift in the loop-top region is due toupflowing plasma originating from the jet. Both hard X-ray and soft X-rayemission from RHESSI were only seen as footpoint brightenings during theimpulsive phase of the flare, then, soft X-ray emission moves to the loop-topin the decay phase. Based on the temperature and density measurements andtheoretical cooling models, the temperature evolution of the flare arch isconsistent with impulsive heating during the jet eruption followed byconductive cooling via evaporation and minor prolonged heating in the top ofthe fan loop. Investigating the magnetic field topology and squashing factormap from SDO/HMI, we conclude that the observed magnetic-fan flaring arch ismostly heated from low atmospheric reconnection accompanying the jet ejection,instead of from reconnection above the arch as expected in the standard flaremodel.

A Solar Magnetic-fan Flaring Arch Heated by Non-thermal Particles and Hot Plasma from an X-ray Jet Eruption