Escape of Flare-accelerated Particles in Solar Eruptive Events
Masson, S., S. K. Antiochos, and C. R. DeVore, Escape of Flare-accelerated Particles in Solar Eruptive Events, ApJ, 884, 143 (2019) (ADS)
(click on the image for a larger version)
The "escape" of impulsive SEPs from a flare site has always been a
problem for CSHKP models.
Viewed in 2.5D, as in an
earlier cartoon,
no escape at all is possible except on the MHD time scale
of the plasmoid eruption.
How then does one promptly populate a propagation cone that may extend
60°?
The answer put forward here is the usual one: allow sufficient magnetic
reconnection and the particles can appear to cross field line quite freely.
That provides a sufficient explanation within the confines of the
"standard model in 3D", it seems.
The "cartoon" shown here is not really a cartoon, just the photospheric
flow field assumed for the numerical simulations described in the paper.
The simulations in a sense replace any need for a cartoon, and the
paper links beautiful movies showing how the process evolves.
The "escape" of impulsive SEPs from a flare site has always been a problem for CSHKP models. Viewed in 2.5D, as in an earlier cartoon, no escape at all is possible except on the MHD time scale of the plasmoid eruption. How then does one promptly populate a propagation cone that may extend 60°? The answer put forward here is the usual one: allow sufficient magnetic reconnection and the particles can appear to cross field line quite freely. That provides a sufficient explanation within the confines of the "standard model in 3D", it seems.
The "cartoon" shown here is not really a cartoon, just the photospheric flow field assumed for the numerical simulations described in the paper. The simulations in a sense replace any need for a cartoon, and the paper links beautiful movies showing how the process evolves.