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

Investigating the early-stage evolution of an erupting flux rope from the Sunis important to understand the mechanisms of how it looses its stability andits space weather impacts. Our aim is to develop an efficient scheme fortracking the early dynamics of erupting solar flux ropes and use the algorithmto analyse its early-stage properties. The algorithm is tested on a data-drivensimulation of an eruption that took place in active region AR12473. Weinvestigate the modelled flux rope's footpoint movement and magnetic fluxevolution and compare with observational data from the Solar DynamicsObservatory's Atmospheric Imaging Assembly in the 211 $\unicode{x212B}$ and1600 $\unicode{x212B}$ channels. To carry out our analysis, we use thetime-dependent data-driven magnetofrictional model (TMFM). We also performanother modelling run, where we stop the driving of the TMFM midway through theflux rope's rise through the simulation domain and evolve it instead with azero-beta magnetohydrodynamic (MHD) approach. The developed algorithmsuccessfully extracts a flux rope and its ascend through the simulation domain.We find that the movement of the modelled flux rope footpoints showcasessimilar trends in both TMFM and relaxation MHD run: they recede from theirrespective central location as the eruption progresses and the positivepolarity footpoint region exhibits a more dynamic behaviour. The ultravioletbrightenings and extreme ultraviolet dimmings agree well with the models interms of their dynamics. According to our modelling results, the toroidalmagnetic flux in the flux rope first rises and then decreases. In ourobservational analysis, we capture the descending phase of toroidal flux. Inconclusion, the extraction algorithm enables us to effectively study the fluxrope's early dynamics and derive some of its key properties such as footpointmovement and toroidal magnetic flux.

The Automatic Identification and Tracking of Coronal Flux Ropes -- Part I: Footpoints and Fluxes