Thermal instability in post-flare plasmas

Details Thermal instability in post-flare plasmas Thermal instability in post-flare plasmas

May 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977phdt.........2a&link_type=abstract

Ph.D. Thesis Stanford Univ., CA.

Astronomy and Astrophysics

Astronomy

Boundary Value Problems, Mathematical Models, Solar Prominences, Solar Wind, Thermal Instability, Chromosphere, Equations Of Motion, Heat Transfer, Magnetohydrodynamic Flow, Perturbation, X Ray Astronomy

Scientific paper

The cooling of post flare plasmas was investigated and a one dimensional model developed for active loop prominences, taking into consideration motion and heat fluxes parallel to the magnetic field. Included in the model are the effects of gravity, the geometry of the field, and conduction losses to the chromosphere. Calculations using the computer code developed and a two-step time differencing scheme indicate that the non-uniform cooling of the post-flare corona can be understood as a direct consequence of the temperature and density dependence of the radiative losses from a high-temperature solar plasma.

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