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

Coronal dimmings, localized regions of reduced emission in the EUV and softX-rays, are interpreted as density depletions due to mass loss during the CMEexpansion. They contain crucial information on the early evolution of CMEs lowin the corona. For 62 dimming events, characteristic parameters are derived,statistically analyzed and compared with basic flare quantities. On average,coronal dimmings have a size of $2.15\times10^{10}$ km$^{2}$, contain a totalunsigned magnetic flux of $1.75\times10^{21}$ Mx, and show a total brightnessdecrease of $-1.91\times10^{6}$ DN, which results in a relative decrease of$\sim$60% compared to the pre-eruption intensity level. Their main evacuationphase lasts for $\sim$50 minutes. The dimming area, the total dimmingbrightness, and the total unsigned magnetic flux show the highest correlationwith the flare SXR fluence ($c\gtrsim0.7$). Their corresponding timederivatives, describing the dimming dynamics, strongly correlate with the GOESflare class ($c\gtrsim 0.6$). For 60% of the events we identified coredimmings, i.e. signatures of an erupting flux rope. They contain 20% of themagnetic flux covering only 5% of the total dimming area. Secondary dimmingsmap overlying fields that are stretched during the eruption and closed down bymagnetic reconnection, thus adding flux to the erupting flux rope via magneticreconnection. This interpretation is supported by the strong correlationbetween the magnetic fluxes of secondary dimmings and flare reconnection fluxes($c=0.63\pm0.08$), the balance between positive and negative magnetic fluxes($c=0.83\pm0.04$) within the total dimmings and the fact that for strong flares($>$M1.0) the reconnection and secondary dimming fluxes are roughly equal.

Statistics of coronal dimmings associated with coronal mass ejections. I. Characteristic dimming properties and flare association