Coronal Mass Ejection (CME) - CESRA: Community of European Solar Radio Astronomers

A 19-day solar radio burst: a corotating radio reservoir in the outer corona by Vratislav Krupar et al.

June 16, 2026

Solar radio astronomers are used to type IV bursts as the long afterglow of eruptive activity: broadband continua, often polarized, produced by energetic electrons trapped in post-eruption magnetic structures. But “long” usually means minutes to hours, sometimes longer in exceptional cases. The event reported by Krupar et al. 2026 changes that scale. A hectometric type IV continuum between about 0.5 and 3 MHz was observed over nearly 19 days, from […]

Technical Readiness of MeerKAT for Solar Observations and Initial Science Results by D. Kansabanik et al.

March 31, 2026

Solar radio emissions offer unique diagnostic insights into the solar corona. However, their dynamic and multiscale nature, along with variations spanning several orders of magnitude in intensity, pose significant observational challenges. To date, at gigahertz frequencies, MeerKAT (Jonas & MeerKAT Team 2016) stands out globally for its intrinsic ability to produce high-fidelity, spectroscopic snapshot images of the Sun. This is enabled primarily by its dense core, high sensitivity, and broad […]

Signatures of Confined and Eruptive Solar Flares in Microwave Spectra by E. W. Cliver et al.

January 6, 2026

Solar flares are generally divided into two classes: eruptive flares (with associated coronal mass ejections; CMEs, see previous CME nuggets by CESRA) and confined flares that lack CMEs. Because eruptive flares are the principal source of major space weather effects at Earth, relatively little attention was paid to confined flares until the great sunspot group of October 2014, designated NOAA 12192, passed across the solar disk giving rise to 35 […]

On the limitations of using metric radio bursts as diagnostic tools for interplanetary coronal mass ejections by J. Kandekar et al.

September 30, 2025

Our Sun is constantly active, and much of its activity, like Solar Flares and Coronal Mass Ejections, is driven by its Magnetic Fields. However, one cannot directly estimate this magnetic field; one needs to employ various observational and radio techniques to estimate these magnetic fields (White 2004; Gopalswamy 2006). While radio-based techniques have been used to explore coronal magnetic fields in localised regions (e.g., using band-splitting in type II bursts; […]

Spectral cleaving in solar type II radio bursts: Observations and interpretation by A. Koval et al.

December 3, 2024

Solar eruptive events, such as flares and coronal mass ejections (CMEs), can generate shock waves that propagate through the solar corona. These shock waves accelerate electrons, leading to Langmuir waves that are then converted into radio emission of type II solar bursts, which are radio signatures of these shocks. On solar spectrograms, type II bursts are typically characterized by fundamental and harmonic lanes drifting from high to low frequencies within […]