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

We present observations and magnetic field modeling of the large polar crownprominence that erupted on 2010 December 6. Combination of SDO/AIA andSTEREO$\_$Behind/EUVI allows us to see the fine structures of this prominenceboth at the limb and on the disk. We focus on the structures and dynamics ofthis prominence before the eruption. This prominence contains two parts: anactive region part containing mainly horizontal threads, and a quiet Sun partcontaining mainly vertical threads. On the northern side of the prominencechannel, both AIA and EUVI observe bright features which appear to be the lowerlegs of loops that go above then join in the filament. Filament materials areobserved to frequently eject horizontally from the active region part to thequiet Sun part. This ejection results in the formation of a dense-columnstructure (concentration of dark vertical threads) near the border between theactive region and the quiet Sun. Using the flux rope insertion method, wecreate non-linear force-free field models based on SDO/HMI line-of-sightmagnetograms. A key feature of these models is that the flux rope hasconnections with the surroundings photosphere, so its axial flux varies alongthe filament path. The height and location of the dips of field lines in ourmodels roughly replicate those of the observed prominence. Comparison betweenmodel and observations suggests that the bright features on the northern sideof the channel are the lower legs of the field lines that turn into the fluxrope. We suggest that plasma may be injected into the prominence along thesefield lines. Although the models fit the observations quiet well, there arealso some interesting differences. For example, the models do not reproduce theobserved vertical threads and cannot explain the formation of the dense-columnstructure.

Observations and Magnetic Field Modeling of a Solar Polar Crown Prominence