Modeling Properties of Chromospheric Evaporation Driven by Thermal Conduction Fronts from Reconnection Shocks

An angular but colorful cartoon in the general genre of CSHKP, but following the idea that Longcope-Bradshaw_2010ApJ...718.1491L_FLA.html physics could help to understand the "evaporation" flow morphology - a good idea, why not try it? The downside of such a model is that it appears to require high densities. The Archivist's preference would be a model that could embrace the impulsive phase, where there is no reason to think that coronal structure involved has any finite value of plasma beta. In the standard cartoon, the CME blows the field open, and the resulting outward flow should exhaust the plasma quite rapidly. Thus the inward flow driving the reconnection would have a low density. Note that it's harder to measure density where it is low, especially in an optically thin medium. All we have observationally here is upper limits, basically, from the existing X-ray and EUV imaging spectroscopy.