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 Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

We present data analysis and interpretation of an M1.4-class flare observedwith the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) on April30, 2002. This event, with its footpoints occulted by the solar limb, exhibitsa rarely observed, but theoretically expected, double-source structure in thecorona. The two coronal sources, observed over the 6-30 keV range, appear atdifferent altitudes and show energy-dependent structures with the higher-energyemission being closer together. Spectral analysis implies that the emission athigher energies in the inner region between the two sources is mainlynonthermal, while the emission at lower energies in the outer region isprimarily thermal. The two sources are both visible for about 12 minutes andhave similar light curves and power-law spectra above about 20 keV. Theseobservations suggest that the magnetic reconnection site lies between the twosources. Bi-directional outflows of the released energy in the form ofturbulence and/or particles from the reconnection site can be the source of theobserved radiation. The spatially resolved thermal emission below about 15 keV,on the other hand, indicates that the lower source has a larger emissionmeasure but a lower temperature than the upper source. This is likely theresult of the differences in the magnetic field and plasma density of the twosources.

Double Coronal Hard and Soft X-ray Source Observed by RHESSI: Evidence for Magnetic Reconnection and Particle Acceleration in Solar Flares