Hydromagnetic wave heating of the galactic corona

Computer Science – Sound

Scientific paper

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Coronas, Galactic Structure, Interstellar Gas, Magnetohydrodynamic Waves, Plasma Heating, Abundance, Astronomical Models, Energy Dissipation, Gas Density, Halos, Plasma Temperature, Stellar Winds, Wave Degradation

Scientific paper

The rate at which hydromagnetic wave energy is dissipated in a galactic corona will be a very sensitive function of temperature when the dissipation occurs primarily through the non-linear decay of Alfvén waves by the production of sound waves. In wave driven wind models of a corona the large dependence of the dissipation rate on temperature can lead to the temperature being an extremely slowly varying function of density, in harmony with the very uniform observed C IV to Si IV abundance ratios in the galactic halo gas.

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