A new study in Nature Communications (2026) uses LOFAR imaging spectroscopy to identify spike-like repeating radio burst pairs in the solar corona — a previously unknown class of fine-scale emission i...

The solar atmosphere is a turbulent and magnetized environment, with the release of magnetic energy readily manifesting as emission across the electromagnetic spectrum. Solar radio emission dominates ...

Decrypting the behaviour of large-scale flows in the Sun, namely the differential rotation and the meridional circulation, is detrimental to the understanding of the evolution of the solar magnetic fi...

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 st...

Solar flares are the most explosive energy-release events in the solar corona, leading to intense particle acceleration, plasma heating and bulk plasma motions on short timescales.

Solar flares are the most explosive energy-release events in the solar corona, leading to intense particle acceleration, plasma heating, and bulk plasma motions on short timescales. Core questions dur...

The Sun is not known for being quiet.

The shape, size and electron density (Ne) of the corona varies with the sunspot cycle, which is now very well established by white-light observations. In our study, we investigated the ‘quiet’ solar c...

Magnetic reconnection, a fundamental process in astrophysical environment plasma is believed to facilitate the release of energy stored in the magnetic field. However, where the magnetic reconnections...

Microwave solar polarization observations give us information about the magnetic field of the solar atmosphere. They are important for understanding the various solar activity phenomena and emission m...

The Sun is the main source of space weather, and one type of solar event that is critical to space weather is a coronal mass ejection. Coronal mass ejections (CMEs) are large eruptions of magnetized p...

Type III solar radio bursts, which appear as characteristic frequency-drifting features on radio dynamic spectra, are generated by energetic beams of electrons originating in solar active regions and ...

Type II and type III bursts are generated, via the plasma emission mechanism, when beams of suprathermal electrons interact with the ambient plasma generating radio emissions at the plasma frequency f...

YouTube video by NASA Space News

Type III solar radio bursts observed by NASA’s Parker Solar Probe may reveal large-scale magnetic-field disturbances and switchback-like structures near the Sun, according to a study published in The…

Typically, solar radio bursts like these last a few hours to days. But this one was different.

EUV (EIT) waves are wavelike disturbances of enhanced extreme ultraviolet (EUV) emission that propagate away from an eruptive region. Recent years have seen much debate over their nature, with three m...

Solar type II radio bursts are slow-drifting emissions in radio dynamic spectra, traditionally interpreted as signatures of shock waves driven by fast coronal mass ejections (CMEs). They provide the p...

Program and timetable Working Group 1: 1A: LowAtmosphere/ARs & 1B Fine structures/QPPs Group leaders: Alexander Nindos + Surajit Mondal Working Group 2: Solar flares Group leader...

Solar radio emission is produced in the turbulent medium of the solar atmosphere, and its observed properties (source position, size, time profile, polarization, etc.) are significantly affected by th...

A coronal mass ejection (CME) is a phenomenon which produces large-scale ejections of mass and magnetic field from the lower corona into the interplanetary space (e.g. Forbes, 2000). The ejection of C...

Comet 2I/Borisov was only the second interstellar object known to have entered the solar system. The highly eccentric, hyperbolic orbit of 2I/Borisov and its high inclination to the ecliptic plane dem...

Solar radio bursts are intrinsically linked to the motion of their emitting source through the coronal and heliospheric plasma. Electron transport is mostly confined to magnetic field lines. These ele...

Type II radio bursts, produced near the local plasma frequency and/or its harmonic by energetic electrons accelerated by shock waves moving outward through the inner heliosphere, have long been recogn...

Solar radio bursts and their fine spectral structures contain key physical information related to plasma instabilities, high-energy particle acceleration, and other important processes. They therefore...

The Sun routinely produces energetic electrons in its outer atmosphere that subsequently travel through interplanetary space. These electron beams generate Langmuir waves in the background plasma, pro...

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, pos...

During encounter 2 of NASA’s PSP mission there was a large amount of radio activity and, in particular, a noise storm of frequent, small type III bursts from 31 March to 6 April 2019. Our aim is to in...

Solar radio spikes are short duration, narrowband radio bursts that are signature of the acceleration of non-thermal electrons in solar flares. They are observed over a wide range of frequencies from ...

Type II radio bursts are slow-drifting and long-lasting radio emission produced by nonthermal electrons accelerated at shocks propagating through the solar corona and interplanetary medium (Nelson & M...

Solar type II bursts are sporadic emissions characterized by their narrow bandwidth and slow frequency drift in dynamic spectra ( Nelson & Melrose, 1985 ; Vršnak & Cliver 2008 ; Nindos et al. 2008 ; P...

The magnetic fields of the Sun govern the solar corona structure where the solar wind emanates and further accelerates supersonically. Therefore, the accurate observational data about the topology, an...

The acceleration of charged particles is an ubiquitous phenomenon in solar flares. Non-thermal electrons are especially probed by their hard X-ray (HXR) and radio emissions. Most flare analyses concer...

For a mission that has just entered its primary science phase, Solar Orbiter has already produced many remarkable results. Released on December 14, 2021, a special issue of Astronomy and Astrophysics ...

Langmuir-Slow extraordinary mode (L-SE) waves have been routinely observed in the Solar wind and in Earth’s electron foreshock since the early age of the space exploration. They are intimately connect...

The plasma density and magnetic field in the upper solar corona and inner heliosphere are not sufficient to produce detectable bremsstrahlung hard X-ray or gyrosynchrotron microwave emissions, making ...

A solar radio burst (SRB) is the intense solar radio emission often related to a solar flare and one of the possibly extreme space weather events which may affect Earth’s ionosphere and signal propaga...

Filaments (or prominences) are “clouds” of cool (<104 K) material suspended in the solar corona by up to tens of megameters above the photosphere, and they can be broadly divided into quiescent filame...

Practically all solar phenomena observed in radio wavelengths have their counterpart in other regions of the electromagnetic spectrum. Metric solar bursts are an exception to the above statement. Alth...

Solar radio bursts (SRBs) are some of the most interesting signatures of solar activity. Their correlation with large solar eruptions and well-documented disruption to technological infrastructure esp...

Filaments (or prominences) are “clouds” of cool (<104 K) material suspended in the solar corona by up to tens of megameters above the photosphere, and they can be broadly divided into quiescent filame...

Solar flares, the most powerful magnetic explosions in our solar system, are often accompanied by intense bursts of radio emission known as type III solar radio bursts. These bursts provide valuable c...

A solar radio burst (SRB) is the intense solar radio emission often related to a solar flare and one of the possibly extreme space weather events which may affect Earth’s ionosphere and signal propaga...

Type III bursts are usually described as a two-step process: energetic electrons excite Langmuir waves, which are then converted into radio emission near the plasma frequency (Ginzburg & Zhelezniakov ...

The plasma density and magnetic field in the upper solar corona and inner heliosphere are not sufficient to produce detectable bremsstrahlung hard X-ray or gyrosynchrotron microwave emissions, making ...

The (sub)millimeter radiation of solar flares, explosive events detected as brightenings across the electromagnetic spectrum, is poorly understood ( Krucker et al. 2013 ) . The major limit of the prev...

The solar radio spikes can provide detailed information about plasma processes in solar flares on kinetic scales. Among them, the decimetric spikes belong to the most interesting ones because they are...