Wild, J. P. and S. F. Smerd, Radio Bursts from the Solar Corona, Annual Review of Astronomy and Astrophysics, 10, 159 (1972) (ADS)
(click on the image for a larger version)
Not a flare cartoon as such, this nevertheless introduces an important
subject: the use of energetic particles as tracers of the coronal
magnetic field in and near flares.
The metric type III, V, and U bursts all are in the category of
"fast-drift bursts," identified by the Australian radio astronomers with
beams of weakly relativistic electrons.
These electrons can quickly appear at one A.U. to be
counted directly by in-situ electron detectors, so they show
that their field lines are open and connect to the low corona.
But what does this really mean, and which field lines are we talking about?
Note that in this cartoon it is not the standard current-sheet
geometry associated with magnetic reconnection (CSHKP),
but a simple coronal null
instead (at least in 2D) via a spine field line and a pseudo-streamer.
See the Masson cartoon for a more
colorful version of this.
Not a flare cartoon as such, this nevertheless introduces an important subject: the use of energetic particles as tracers of the coronal magnetic field in and near flares. The metric type III, V, and U bursts all are in the category of "fast-drift bursts," identified by the Australian radio astronomers with beams of weakly relativistic electrons. These electrons can quickly appear at one A.U. to be counted directly by in-situ electron detectors, so they show that their field lines are open and connect to the low corona. But what does this really mean, and which field lines are we talking about? Note that in this cartoon it is not the standard current-sheet geometry associated with magnetic reconnection (CSHKP), but a simple coronal null instead (at least in 2D) via a spine field line and a pseudo-streamer. See the Masson cartoon for a more colorful version of this.