Strauss, Federico M. and Michael D. Papagiannis, A Model for the Source of Solar-Flare X-Rays, ApJ, 164, 369 (1971) (ADS)
(click on the image for a larger version)
An early use of
Sturrock's model, a.k.a.
the S in CSHKP, aimed at
locating the X-ray sources in solar flares.
This was not long after Kane had introduced the "impulsive phase" as a
guideline to hard X-ray emission, and Neupert had introduced what is now
called the Neupert effect.
In fact, this (at the time of writing) seems to have been the first
full-fledged cartoon in this genre of 2D reconnection scenarios.
Hirayama's more 3-dimensional
view did not arrive until 1974.
In this era solar physicists were just coming around to the idea of
thinking about solar flares in terms of their X-ray signatures
(but of course ionospheric physicists had always known about this).
The model calculations in the paper only dealt with thermal free-free
emission, at temperatures ranging up to almost 60 MK, to explain the
OGO-5 hard X-ray observations of a nice contemporaneous flare
(SOL1968-06-20T17).
An early use of Sturrock's model, a.k.a. the S in CSHKP, aimed at locating the X-ray sources in solar flares. This was not long after Kane had introduced the "impulsive phase" as a guideline to hard X-ray emission, and Neupert had introduced what is now called the Neupert effect. In fact, this (at the time of writing) seems to have been the first full-fledged cartoon in this genre of 2D reconnection scenarios. Hirayama's more 3-dimensional view did not arrive until 1974. In this era solar physicists were just coming around to the idea of thinking about solar flares in terms of their X-ray signatures (but of course ionospheric physicists had always known about this). The model calculations in the paper only dealt with thermal free-free emission, at temperatures ranging up to almost 60 MK, to explain the OGO-5 hard X-ray observations of a nice contemporaneous flare (SOL1968-06-20T17).