Unusual Type III Burst Dynamics Produced by Diverging Magnetic Fields

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Introduction

Type III solar radio bursts are widely believed to be caused by electron beams accelerated away from the Sun during solar flares. Fast electrons stimulate oscillations in the ambient plasma, which in turn produce radio emission. This plasma emission occurs at specific frequencies that are proportional to the square root of the ambient electron density. The plasma density in the solar corona generally decreases outwards from the solar surface. The emission frequency is therefore related to the height that corresponds to the requisite background density, and type III bursts are characterized by a rapid drift to lower frequencies as the beams move outward.

Source Region Splitting

A series of type III bursts have recently been observed to exhibit a curious splitting behavior by the Murchison Widefield Array (MWA), a new and very powerful low-frequency radio interferometer (Ref. [1]). In these bursts the source region splits from one component at higher frequencies (smaller heights), into two increasingly-separated components at lower frequencies (larger heights). The two components also repetitively move apart at a few tenths of light speed in observations at individual frequencies. This motion, shown in Figure 1, lasts around 2 seconds and occurs many times over several minutes.

Figure 1: Source splitting motion at 108 MHz, beginning at 2015/09/21 05:16:53.70 UT. The dashed line in the left panel denotes the slit used for kinematic analysis (Ref. [1]). The two solid black contours are at 0.010 and 0.015 SFU px^-1, and the values in the lower right of each panel note the integrated flux densities in SFU. The star represents the X-ray flare site, the solid semicircle represents the optical disk, the dotted semicircle represents the Newkirk-model limb at 108 MHz, and the white ellipse represents the synthesized beam (resolution element).

Magnetic Field Configuration

Extreme ultraviolet (EUV) jets observed by the Solar Dynamics Observatory/AIA immediately follow the radio bursts. These thermal plasma ejections and the type III electron beams follow particular trajectories within the coronal magnetic field, and previous studies have demonstrated alignment between the two (e.g. Ref. [2]). The EUV jets trace out a region where the magnetic field diverges rapidly around a null point. This configuration is a type of quasi-separatrix layer (QSL), generally meaning a region where the field connectivity changes drastically within a small area. Several common features of null point QSLs are identified in Figure 2, which compiles all of the EUV jet trajectories into one persistence map.

Figure 2: A) Maximum value persistence maps for AIA 304 (top) and 171 A (bottom). B) Column A subtracted by median backgrounds. C) A further-processed version of Column B (top) with annotations labeling several QSL features. Such images compile all of the EUV jet trajectories from immediately after the radio bursts by plotting the maximum value a given pixel achieves over a 20-min period.

References

[1] "Type III Solar Radio Burst Source Region Splitting Due to a Quasi-Separatrix Layer"

[2] "Tracing Electron Beams in the Sun's Corona with Radio Dynamic Imaging Spectroscopy"