Observing Flux Rope Formation During the Impulsive Phase of a Solar Eruption
Cheng, X., J. Zhang, Y. Liu, and M. D. Ding, Observing Flux Rope Formation During the Impulsive Phase of a Solar Eruption, ApJ, 732, L25 (2011) (ADS)
(click on the image for a larger version)
Do the magnetic fields in the CSHKP current sheet actually
connect out into the heliosphere?
This question cannot readily be answered by a 2D cartoon, as shown here.
Note that this well-cited paper aims to describe an erupting flux rope
as having formed prior to the reconnection process.
Radio type III bursts, due to weakly relativistic electrons with high speeds
and small gyroradii, probe magnetic connectivity as well as any diagnostic
emission can.
The original Wild & Smerd point
of view of this connectivity is that the "flare reconnection" current
sheet does link out into the heliosphere and that the electron streams
originate there.
The Archivist does not like this, nor the more contrived modern
"particle escape" cartoons.
This seems to be an unsolved problem.
The perhaps puzzling numbers (211, 192 etc.) refer to AIA passbands.
Do the magnetic fields in the CSHKP current sheet actually connect out into the heliosphere? This question cannot readily be answered by a 2D cartoon, as shown here. Note that this well-cited paper aims to describe an erupting flux rope as having formed prior to the reconnection process. Radio type III bursts, due to weakly relativistic electrons with high speeds and small gyroradii, probe magnetic connectivity as well as any diagnostic emission can. The original Wild & Smerd point of view of this connectivity is that the "flare reconnection" current sheet does link out into the heliosphere and that the electron streams originate there. The Archivist does not like this, nor the more contrived modern "particle escape" cartoons. This seems to be an unsolved problem.
The perhaps puzzling numbers (211, 192 etc.) refer to AIA passbands.