An Introduction to Theory and Models of CMEs, Shocks, and Solar Energetic Particles
Mikić, Z. and M. A. Lee, An Introduction to Theory and Models of CMEs, Shocks, and Solar Energetic Particles, Space Sci. Rev., 123, 57-80 (2006) (ADS)
(click on the image for a larger version)
Another version of a well-known cartoon, due originally (I believe) to
Hilary Cane but well-exploited by many others.
It shows how a CME-driven bow shock may accelerate high-energy particles in the
corona or heliosphere via diffusive shock acceleration.
This theory explains several features of the observations.
In this version one can see the helical flux rope pushing on essentially open field
lines, whose wiggles are associated with particle acceleration.
In common with many versions of this cartoon, it looks a bit weird at
the bottom middle of the figure - intuitively one would not expect
the shock to be strong at this position, but there it is represented
far from its driver.
Where is the possibly important "quasi-perp" condition to be found?
One would expect the highest Mach number and
strongest acceleration right at the bow of the CME's radial motion,
of course, without that constraint.
The numbers refer to (1) the ambient solar wind, (2)
the region in which the accelerated ions are supposed to excite
turbulence, and (3) the downstream region in which the shock has
heated the medium.
Another version of a well-known cartoon, due originally (I believe) to Hilary Cane but well-exploited by many others. It shows how a CME-driven bow shock may accelerate high-energy particles in the corona or heliosphere via diffusive shock acceleration. This theory explains several features of the observations. In this version one can see the helical flux rope pushing on essentially open field lines, whose wiggles are associated with particle acceleration. In common with many versions of this cartoon, it looks a bit weird at the bottom middle of the figure - intuitively one would not expect the shock to be strong at this position, but there it is represented far from its driver. Where is the possibly important "quasi-perp" condition to be found? One would expect the highest Mach number and strongest acceleration right at the bow of the CME's radial motion, of course, without that constraint.
The numbers refer to (1) the ambient solar wind, (2) the region in which the accelerated ions are supposed to excite turbulence, and (3) the downstream region in which the shock has heated the medium.