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

Non-potential magnetic energy promptly released in solar flares is convertedto other forms of energy. This may include nonthermal energy offlare-accelerated particles, thermal energy of heated flaring plasma, andkinetic energy of eruptions, jets, up/down flows, and stochastic (turbulent)plasma motions. The processes or parameters governing partitioning of thereleased energy between these components is an open question. How thesecomponents are distributed between distinct flaring loops and what controlsthese spatial distributions is also unclear. Here, based on multi-wavelengthdata and 3D modeling, we quantify the energy partitioning and spatialdistribution in the well observed SOL2014-02-16T064620 solar flare of classC1.5. Nonthermal emissions of this flare displayed a simple impulsivesingle-spike light curves lasting about 20\,s. In contrast, the thermalemission demonstrated at least three distinct heating episodes, only one ofwhich was associated with the nonthermal component. The flare was accompaniedby up and down flows and substantial turbulent velocities. The results of ouranalysis suggest that (i) the flare occurs in a multi-loop system that includedat least three distinct flux tubes; (ii) the released magnetic energy isdivided unevenly between the thermal and nonthermal components in these loops;(iii) only one of these three flaring loops contains an energetically importantamount of nonthermal electrons, while two other loops remain thermal; (iv) theamounts of direct plasma heating and that due to nonthermal electron loss arecomparable; (v) the kinetic energy in the flare footpoints constitute only aminor fraction compared with the thermal and nonthermal energies.

Energy budget of plasma motions, heating, and electron acceleration in a three-loop solar flare