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

Solar filaments/prominences are one of the most common features in thecorona, which may lead to energetic coronal mass ejections (CMEs) and flareswhen they erupt. Filaments are about one hundred times cooler and denser thanthe coronal material, and physical understanding of their material originremains controversial. Two types of scenarios have been proposed: one arguesthat the filament plasma is brought into the corona from photosphere orchromosphere through a siphon or evaporation/injection process, while the othersuggests that the material condenses from the surrounding coronal plasma due tothermal instability. The elemental abundance analysis is a reasonable clue toconstrain the models, as the siphon or evaporation/injection model wouldpredict that the filament material abundances are close to the photospheric orchromospheric ones, while the condensation model should have coronalabundances. In this letter, we analyze the elemental abundances of a magneticcloud that contains the ejected filament material. The corresponding filamenteruption occurred on 1998 April 29, accompanying an M6.8 class soft X-ray flarelocated at the heliographic coordinates S18E20 (NOAA 08210) and a fast halo CMEwith the linear velocity of 1374 km s$^{-1}$ near the Sun. We find that theabundance ratios of elements with low and high First Ionization Potential suchas Fe/O, Mg/O, and Si/O are 0.150, 0.050, and 0.070, respectively, approachingtheir corresponding photospheric values 0.065, 0.081, and 0.066, which does notsupport the coronal origin of the filament plasma.

The Origin of Solar Filament Plasma Inferred from in situ Observations of Elemental Abundances