A Hybrid Fluid - Kinetic Approach to Numerical Models of Solar Coronal Loops

Details A Hybrid Fluid - Kinetic Approach to Numerical Models of Solar Coronal Loops A Hybrid Fluid - Kinetic Approach to Numerical Models of Solar Coronal Loops

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009spd....40.3002b&link_type=abstract

American Astronomical Society, SPD meeting #40, #30.02; Bulletin of the American Astronomical Society, Vol. 41, p.864

Physics

Scientific paper

A hot (T >= 10 MK), though relatively weak, component of coronal emission is predicted by impulsive, nanoflare-type heating models and supporting observational evidence is gradually beginning to accumulate. If such a component of the emission is indeed present then it will arise from high temperature, low density plasma, prior to the onset of significant chromospheric evaporation. High temperatures and low densities lead to long path lengths and free-streaming electrons. Under such circumstances we may expect classical fluid treatments of physical processes such as thermal conduction to break down. Kinetic effects, such as flux limiting and non-local contributions, then become extremely important in determining the coronal energy balance.
The enormous variation in the relevant length scales throughout the solar corona, and the underlying atmospheric layers, prohibits a large scale treatment by a purely kinetic approach. However, a comprehensive treatment of the appropriate physics is amenable to a combined fluid and kinetic approach.
Here I present progress on the development of just such a model and results that demonstrate the failings of the purely fluid approach and the ability of the new model to overcome them.

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