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 Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

We present SDO/AIA observation of three types of fast-mode propagatingmagnetosonic waves in a GOES C3.0 flare on 2013 April 23, which was accompaniedby a prominence eruption and a broad coronal mass ejection (CME). During thefast rising phase of the prominence, a large-scale dome-shaped extremeultraviolet (EUV) wave firstly formed ahead of the CME bubble and propagated ata speed of about 430 km/s in the CME's lateral direction. One can identify theseparation process of the EUV wave from the CME bubble. The reflection effectof the on-disk counterpart of this EUV wave was also observed when itinteracted with a remote active region. Six minutes after the first appearanceof the EUV wave, a large-scale quasi-periodic EUV train with a period of about120 seconds appeared inside the CME bubble, which emanated from the flareepicenter and propagated outward at an average speed up to 1100 km/s. Inaddition, another narrow quasi-periodic EUV wave train was observed along aclosed-loop system connecting two adjacent active regions, which also emanatedfrom the flare epicenter, propagated at a speed of about475 km/s and with aperiod of about 110 seconds. We propose that all the observed waves arefast-mode magnetosonic waves, in which the large-scale dome-shaped EUV waveahead of the CME bubble was driven by the expansion of the CME bubble, whilethe large-scale quasi-periodic EUV train within the CME bubble and the narrowquasi-periodic EUV wave train along the closed-loop system were excited by theintermittent energy-releasing process in the flare. Coronal seismologyapplication and energy carried by the waves are also estimated based on themeasured wave parameters.

CME-Driven and Flare-Ignited Fast Magnetosonic Waves Successively Detected in a Solar Eruption