Solar spicules were discovered by the Jesuit priest Angelo Secchi in 1877. They are small plasma jets of a few hundred kilometers in diameter that are launched to heights >10 Mm with speeds ranging from a few 10s of km/s to >100 km/s. Individually they have lifetimes of a few minutes. They occur in the chromospheric network over the entirety of the Sun. Early estimates (Beckers 1972) suggested that spicules […]
Solar flares accelerate energetic electrons that escape into interplanetary space, guided by the Parker spiral magnetic field, and are responsible for the generation of the interplanetary Type III solar radio bursts. With multiple spacecraft now in orbit around the Sun (see e.g. Musset et al 2021), we are in a unique position of observing the propagation of radio emission through the heliosphere from multiple vantage points. Recent study by Clarkson […]
Plasmoids (or magnetic islands) are believed to play an important role in the onset of fast magnetic reconnection and particle acceleration during solar flares and eruptions. Direct imaging of flare current sheets and formation/ejection of multiple plasmoids in extreme ultraviolet (EUV) images, along with simultaneous X-ray and radio observations, provides significant insights into the mechanisms driving particle acceleration in solar flares. Previous studies have proposed that decimetric radio bursts and […]
Type III radio bursts are the most powerful and common type of solar radio bursts, shifting rapidly from high to low frequencies. In addition to the fast frequency drift from high to low frequencies, the fundamental–harmonic (F-H) frequency pairs’ structure in their dynamic spectra is the other most important observed feature of solar type III radio bursts. In this Letter, using the radio data observed by PSP during encounter phases […]
Solar radio bursts are an indirect signature of accelerated electron beams from the solar atmosphere. These fast electrons generate Langmuir waves as they propagate through a decreasing plasma density and ultimately lead to the bright broadband radio emissions with a characteristic fast frequency drift in dynamic spectra. Density turbulence in the plasma can modulate this process, producing fine structures such as sub-second, narrowband striae and spikes. These fine structures may […]
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 clues about the acceleration and transport of energetic electrons in the Sun’s atmosphere and beyond. Understanding these bursts is not only crucial for solar physics but also for predicting space weather events that can disrupt our technological infrastructure. A […]
Solar type V radio bursts are broad-band continua associated with type III bursts, which are generally believed to be caused by coronal electron beams. Type V bursts appear sometimes for 0.2 to 3 minutes as a continuum following an intense type III burst or group of bursts. The spectral peak of type V bursts is generally below 100 MHz. The high-frequency edge is below the start frequency of the associated type […]
Type III radio bursts are the most common coherent radio emission produced by the Sun. They are characterized by a rapid drift in time towards lower frequencies and represent an indirect signature of energetic electrons produced at the Sun during a flare and propagating through the plasma of the corona and the interplanetary medium. Type III bursts are observed over a wide range of frequencies ranging from about ∼500 MHz […]
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