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

Chromospheric evaporation is observed as Doppler blueshift during solarflares. It plays one of key roles in dynamics and energetics of solar flares,however, its mechanism is still unknown. In this paper we present a detailedanalysis of spatially-resolved multi-wavelength observations of chromosphericevaporation during an M 1.0 class solar flare (SOL2014-06-12T21:12) using datafrom the NASA's IRIS (Interface Region Imaging Spectrograph) and HMI/SDO(Helioseismic and Magnetic Imager onboard Solar Dynamics Observatory)telescopes, and VIS/NST (Visible Imaging Spectrometer at New Solar Telescope)high-resolution observations, covering the temperature range from 10^4 K to10^7 K. The results show that the averaged over the region Fe XXI blueshift ofthe hot evaporating plasma is delayed relative to the C II redshift of therelatively cold chromospheric plasma by about 1 min. The spatial distributionof the delays is not uniform across the region and can be as long as 2 min inseveral zones. Using vector magnetograms from HMI we reconstruct the magneticfield topology and the quasi-separatrix layer (QSL) and find that the blueshiftdelay regions as well as the H-alpha flare ribbons are connected to the regionof magnetic polarity inversion line (PIL) and an expanding flux rope via asystem of low-lying loop arcades with height < ~4.5 Mm. This allows us topropose an interpretation of the chromospheric evaporation based on thegeometry of local magnetic fields, and the primary energy source associatedwith the PIL.

Relationship between chromospheric evaporation and magnetic field topology in M-class solar flare