Quasi-periodic Fast-mode Magnetosonic Wave Trains Within Coronal Waveguides Associated with Flares and CMEs

TL;DR

This paper discusses the discovery and analysis of quasi-periodic fast-mode magnetosonic wave trains in the solar corona, highlighting their properties, origins, and potential roles in coronal heating and solar wind acceleration.

Contribution

It provides new observational insights into QFPs, including their spatio-temporal characteristics, temperature dependence, and correlation with flares and CMEs.

Findings

QFPs originate from flares and propagate at speeds up to ~2000 km/s.

QFPs can carry sufficient energy fluxes for coronal heating.

QFPs are correlated with radio bursts and may influence solar wind acceleration.

Abstract

Quasi-periodic, fast-mode, propagating wave trains (QFPs) are a new observational phenomenon recently discovered in the solar corona by the Solar Dynamics Observatory with extreme ultraviolet (EUV) imaging observations. They originate from flares and propagate at speeds up to ~2000 km/s within funnel-shaped waveguides in the wakes of coronal mass ejections (CMEs). QFPs can carry sufficient energy fluxes required for coronal heating during their occurrences. They can provide new diagnostics for the solar corona and their associated flares. We present recent observations of QFPs focusing on their spatio-temporal properties, temperature dependence, and statistical correlation with flares and CMEs. Of particular interest is the 2010-Aug-01 C3.2 flare with correlated QFPs and drifting zebra and fiber radio bursts, which might be different manifestations of the same fast-mode wave trains. We also discuss the potential roles of QFPs in accelerating and/or modulating the solar wind.