Editorial: Solar radio bursts and their applications in space weather forecasting

Editorial on the Research Topic
Solar radio bursts and their applications in space weather forecasting

The solar radio burst is a good indicator for energetic particle acceleration and plasma processes in the solar corona and heliosphere. Because radio emission is generated by electron beams at or near the local plasma frequency and its harmonics, radio bursts can provide a direct diagnostic of electron beams, shock formation, and the coronal plasma conditions across spatial and temporal scales that are otherwise difficult to access. For decades, solar radio bursts have been critical for our physical understanding of solar eruptive phenomena. Increasingly, they are also becoming critical tools for space weather forecasting, offering early indicators of eruptive activity, shock propagation, and geoeffective solar–interplanetary disturbances.

This Research Topic, Solar Radio Bursts and Their Applications in Space Weather Forecasting, brings together the contributions that collectively illustrate how detailed radio observations, quantitative analysis, and modeling approaches are strengthening the connection between fundamental radio burst physics and forecasting-oriented applications. The papers span fine-structure studies in the decameter range, statistical assessments of radio–CME–shock relationships, and predictive modeling relevant to solar activity and heliospheric propagation, reflecting the multi-scale nature of space weather research.

A first group of contributions focuses on the microphysics and spectral–temporal properties of solar radio bursts, particularly in the decameter wavelength regime. High-resolution observations of type III bursts reveal how different parts of a single burst trace electron populations with distinct velocities, providing strong observational support for beam-driven plasma emission scenarios and velocity dispersion effects. Complementary studies of fine structures, such as decameter spikes and S-bursts, extend this picture by examining polarization properties, drift rates, durations, and frequency extents in unprecedented detail. These analyses show that even weak and short-lived radio features encode valuable information about coronal plasma conditions, electron beam energetics, and small-scale density inhomogeneities. Together, these works emphasize that fine structures are not merely observational curiosities but are powerful diagnostics of the physical environments in which particle acceleration occurs.

A second theme emerging from this Topic is the link between radio bursts, shocks, and geoeffective solar–interplanetary disturbances. Statistical analyses of type II radio bursts and their associations with coronal mass ejections (CMEs) and interplanetary shocks demonstrate that radio signatures carry predictive information about whether a solar eruption is likely to impact Earth. In particular, the presence and spectral characteristics of type II bursts, including their frequency evolution and cutoff behavior, are shown to correlate with the probability and intensity of geomagnetic responses. These results reinforce the long-recognized role of type II bursts as shock tracers while quantitatively strengthening their relevance for operational space weather forecasting. By grounding statistical correlations in physically motivated radio diagnostics, these studies help bridge the gap between solar observations and near-Earth consequences.

Beyond individual events and correlations, the Topic also highlights the growing role of predictive modeling and data-driven approaches in space weather research. Advances in machine learning and time-series forecasting are illustrated through models designed to predict long-term solar activity indicators, such as sunspot numbers, which form the broader context for eruptive activity and radio burst occurrence. Although not focused on radio emission alone, such predictive frameworks are essential components of space weather systems, as they inform expectations of solar activity levels on cycle timescales. When combined with radio-based diagnostics of eruptive events, these approaches contribute to a more complete forecasting chain, from long-term solar variability to short-term space weather hazards.

An important message conveyed by the six contributions is that solar radio bursts operate at the intersection of fundamental plasma physics and practical forecasting needs. Detailed spectral, temporal, and polarization measurements constrain emission mechanisms and coronal conditions, while statistical and modeling studies translate these constraints into probabilistic assessments of space weather impacts. The diversity of approaches represented here—from single-event case studies to large-sample statistical analyses and predictive modeling—underscores the necessity of integrating multiple methodologies to improve forecast reliability.

Looking forward, the results presented in this Research Topic point toward several promising directions. Continued development of broadband, high-dynamic-range radio instruments will further enhance our ability to resolve fine structures and localize burst sources. At the same time, the incorporation of automated detection, machine learning, and physics-informed models will be essential for handling increasing data volumes and enabling real-time or near-real-time applications. Ultimately, the full forecasting potential of solar radio bursts will be realized through coordinated use of radio observations alongside multi-wavelength remote sensing and in situ measurements.

In summary, the six papers collected in this Research Topic demonstrate how modern solar radio studies are advancing both our physical understanding of energetic processes in the solar atmosphere and our ability to anticipate their impacts on the heliosphere and Earth. By linking fine-scale radio diagnostics to large-scale space weather consequences, this Topic highlights the enduring and evolving role of solar radio bursts in space weather forecasting.

Author contributions

PZ: Writing – review and editing.

Funding

The author(s) declared that financial support was received for this work and/or its publication.

Acknowledgments

PZ acknowledges support for this research by the NASA Living with a Star Jack Eddy Postdoctoral Fellowship Program, administered by UCAR’s Cooperative Programs for the Advancement of Earth System Science (CPAESS) under award 80NSSC22M0097.

Conflict of interest

The author(s) declared that this work was conducted in the absence of any commercial or financial relationships that could be construed as a potential conflict of interest.

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