Nonlinear thermal instability in the solar transition region

Details Nonlinear thermal instability in the solar transition region Nonlinear thermal instability in the solar transition region

Jan 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...324..590k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 324, Jan. 1, 1988, p. 590-605. Navy-NASA-supported research.

Physics

Plasma Physics

18

Cosmic Plasma, Plasma Physics, Solar Corona, Stellar Structure, Thermal Instability, Transition Flow, Astronomical Models, Boundary Value Problems, Interstellar Space, Molecular Clouds, Plasma Temperature, Solar Prominences

Scientific paper

The authors extend their earlier investigation on the initiation and evolution of the radiation-driven thermal instability in an atmosphere similar to the solar transition region. They find that the ultimate state of the medium is highly sensitive to the evolving modal content of the perturbation: both the initial modal composition and the extent of mode coupling determine the final structure of the atmosphere. Previous calculations showed that saturation of the instability occurs quite early, preventing appreciable condensation, when excessive heat is added either directly or by conversion of kinetic energy into internal energy. No anologous perturbation-amplitude threshold exists for the present calculations, in which the internal energy is perturbed locally in coincidence with the density while the global values remain unperturbed. The results show that the condensation process generates highly rotational flows during and after the transition to a new stable state.

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