Weak Solar Radio Bursts from the Solar Wind Acceleration Region Observed by the Parker Solar Probe and Its Probable Emission Mechanism by Ling Chen et al.


The study of solar wind acceleration and coronal heating has been a major challenge in solar physics. The main difficulty is that the collisionless characteristic of high-temperature, thin, and fully ionized coronal plasmas lead to the heating and acceleration of the coronal plasmas to be dominated by wave particle interactions, which are the “elementary processes” of the plasma collective interaction at the kinetic scales of plasma particles. Radio observation becomes […]

An Interactive Visual Tool for the Anisotropic Scattering of Solar Radio Bursts by Daniel L. Clarkson et al


The turbulent heliosphere has a significant effect on the observed characteristics of radio emission produced in, or viewed through, the solar atmosphere. In particular, radio-wave scattering on density irregularities can broaden the observed decay times and source sizes, and shift the apparent source position. Both radio burst observations and simulations have demonstrated that the turbulence is anisotropic, which can explain both the observed decay times and source sizes simultaneously. Considering […]

The physics of solar spectral imaging observations in dm-cm wavelengths and space weather by Tan et al.


Recent years, several new generation solar radio telescopes operating in the centimeter decimeter (dm-cm) wavelengths have emerged in the world, including the Mingantu Spectral Radioheliograph (MUSER, 0.4-15GHz) (Yan et al. 2021), the Expanded Owens Valley Solar Array (EOVSA, 1-18GHz) (Gary et al. 2018), and the Siberian Radio Heliograph (SRH, 3-24GHz) (Altyntsev et al. 2020). Due to the fact that the solar radio emission in dm-cm wavelengths mainly originates from the […]

Source positions of an interplanetary type III radio burst and anisotropic radio-wave scattering by X. Chen et al.


Interplanetary solar radio type III bursts provide the means to remotely study and track energetic electrons propagating in the interplanetary medium. Due to the lack of direct radio source imaging, several methods have been developed to determine the source positions from space-based observations. Moreover, none of the methods consider the propagation effects of anisotropic radio-wave scattering, which would strongly distort the trajectory of radio waves, delay their arrival times, and […]

Anisotropic density turbulence variation from the low corona to 1 au as deduced from solar radio observations by E. Kontar et al.


Density turbulence in the solar corona and solar wind is evident via the properties of solar radio bursts; angular scattering-broadening of extra-solar radio sources observed through the solar atmosphere, and can be measured in-situ in the solar wind. A viable density turbulence model should simultaneously explain all three types of density fluctuation observations. Solar radio bursts (e.g. Type I, II, III) observed below ~1 GHz are produced predominantly via plasma […]

Separating the effects of earthside and far side solar events by Silja Pohjolainen et al.


During times of high solar activity flares and coronal mass ejections (CMEs) occur close in time, sometimes even simultaneously, and it may be difficult to identify their source regions. Especially fast CMEs that are observed as propagating fronts high in the corona,  can originate from a region on the Earth-facing side, or from the far side. To determine their origins and direction of propagation, one needs to do a careful […]

Deciphering Faint Gyrosynchrotron Emission from a Coronal Mass Ejection Using Spectropolarimetric Radio Imaging by Devojyoti Kansabanik, Surajit Mondal and Divya Oberoi


Coronal mass ejections (CMEs) are large-scale expulsion of plasma and magnetic fields from the solar corona into the heliosphere. Magnetic field entrained in the CME plasma is crucial to understand their propagation, evolution, and geo-effectiveness. Among the different observables at radio wavelengths, spectral modeling of faint gyrosynchrotron (GS) emission from CME plasma has been regarded as one of the most promising remote observing techniques for estimating spatially resolved CME magnetic […]

A New 6-15 GHz Solar Radio Observation System, by Lei Zhang et al.


In the decimeter to centimeter wavelength, solar radio emission during bursts are generally accepted to be generated by gyrosynchrotron. The typical gyrosynchrotron spectra present reverse-V shapes. And the spectral parameters, including the peak frequency, peak flux and declining spectra etc. can provide crucial information of the bursts. The spectral peak usually appears around 10 GHz. And it is demanded that a continuum observation can cover this frequency range. Meanwhile, the […]

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