Densities Probed by Coronal Type III Radio Burst Imaging
Patrick I. McCauley, Iver H. Cairns, and John Morgan

TL;DR
This study uses low-frequency radio imaging to derive coronal density profiles during solar type III bursts, revealing high densities associated with streamers and discussing propagation effects and electron beam speeds.
Contribution
It provides new coronal density measurements from radio imaging, compares emission assumptions, and discusses propagation effects influencing observed densities.
Findings
Derived electron densities of 1.8 x10^8 cm^-3 at 1.3-1.9 solar radii.
Estimated electron beam speeds between 0.24 and 0.60 c.
High densities are partly due to propagation effects and overdense structures.
Abstract
We present coronal density profiles derived from low-frequency (80-240 MHz) imaging of three type III solar radio bursts observed at the limb by the Murchison Widefield Array (MWA). Each event is associated with a white light streamer at larger heights and is plausibly associated with thin extreme ultraviolet rays at lower heights. Assuming harmonic plasma emission, we find average electron densities of 1.8 x10^8 cm^-3 down to 0.20 x10^8 cm^-3 at heights of 1.3 to 1.9 solar radii. These values represent roughly 2.4-5.4x enhancements over canonical background levels and are comparable to the highest streamer densities obtained from data at other wavelengths. Assuming fundamental emission instead would increase the densities by a factor of 4. High densities inferred from type III source heights can be explained by assuming that the exciting electron beams travel along overdense fibers or…
Peer Reviews
No public reviews on file for this paper yet. If you reviewed it on a platform where reviews are public (OpenReview, ICLR, NeurIPS, ICML), you can paste yours below so the community can read it here.
Videos
No videos yet. Explain this paper in a talk, walkthrough, or lecture? Add one.
