Sub-second time evolution of Type III solar radio burst sources at fundamental and harmonic frequencies

Abstract

Recent developments in astronomical radio telescopes opened new opportunities in imaging and spectroscopy of solar radio bursts at sub-second timescales. Imaging in narrow frequency bands has revealed temporal variations in the positions and source sizes that do not fit into the standard picture of type III solar radio bursts, and require a better understanding of radio-wave transport. In this paper, we utilise 3D Monte Carlo ray-tracing simulations that account for the anisotropic density turbulence in the inhomogeneous solar corona to quantitatively explain the image dynamics at the fundamental (near plasma frequency) and harmonic (double) plasma emissions observed at \sim 32~MHz. Comparing the simulations with observations, we find that anisotropic scattering from an instantaneous emission point source can account for the observed time profiles, centroid locations, and source sizes of the fundamental component of type III radio bursts (generated where f_{pe} \approx 32~MHz). The best agreement with observations is achieved when the ratio of the perpendicular to the parallel component of the wave vector of anisotropic density turbulence is around 0.25. Harmonic emission sources observed at the same frequency (\sim 32~MHz, but generated where f_{pe} \approx 16~MHz) have apparent sizes comparable to those produced by the fundamental emission, but demonstrate a much slower temporal evolution. The simulations of radio-wave propagation make it possible to quantitatively explain the variations of apparent source sizes and positions at sub-second time-scales both for the fundamental and harmonic emissions, and can be used as a diagnostic tool for the plasma turbulence in the upper corona.

arXiv comment17 pages, 6 figures, accepted

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Cited by in corpus (15)

• An Anisotropic Density Turbulence Model from the Sun to 1 au Derived From Radio Observations
• Simulations of radio-wave anisotropic scattering to interpret type III radio bursts measurements by Solar Orbiter, Parker Solar Probe, STEREO and Wind
• Energetic particle activity in AD Leo: Detection of a solar-like type-IV burst
• Coronal mass ejections and type II radio emission variability during a magnetic cycle on the solar-type star $\epsilon$ Eridani
• Characterising coronal turbulence using snapshot imaging of radio bursts in 80-200 MHz
• Source positions of an interplanetary type III radio burst and anisotropic radio-wave scattering
• Quantifying the Magnetic Structure of a Coronal Shock Producing a Type II Radio Burst
• First Frequency-Time-Resolved Imaging Spectroscopy Observations of Solar Radio Spikes
• Solar Radio Spikes and Type IIIb Striae Manifestations of Sub-second Electron Acceleration Triggered by a Coronal Mass Ejection
• Tracing the Heliospheric Magnetic Field via Anisotropic Radio-Wave Scattering
• Interferometric imaging of the type IIIb and U radio bursts observed with LOFAR on 22 August 2017
• Magnetic Field Geometry and Anisotropic Scattering Effects on Solar Radio Burst Observations
• The frequency ratio and time delay of solar radio emissions with fundamental and harmonic components
• Temporally resolved Type III solar radio bursts in the frequency range 3-13 MHz
• Sizes and shapes of sources in solar metric radio bursts