Abstract
The dynamical properties of a realisticthermal-structure interface between a coronal loop and the chromosphere/photosphere are investigated by numerical simulations using acoustic and Alfvénic excitations. These properties are relevant to the end conditions seen by coronal MHD perturbations (e.g., waves or instabilities), in the absence of much slower energetics effects. Analytic studies of coronal-loop hydromagnetics have often made simplifying assumptions about the boundary conditions at the loop base in order to make their calculations tractable. However, in the presence of a transition region and chromosphere with rapidly varying plasma conditions, it is not clear how valid these heuristic assumptions are. In this study, we find that the discontinuous fluid-density model approximately represents the reflection/ transmission scaling with respect to varying transition-region density and temperature (i.e., dynamic impedance) ratios, although it does not quantitatively predict the chromospheric response to wave-like coronal activity. This disagreement is partially due to the finite width of the corona-to-photosphere transition.
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Mok, Y., Van Hoven, G. The solar-surface boundary conditions of coronal magnetic loops. Sol Phys 161, 67–81 (1995). https://doi.org/10.1007/BF00732085
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DOI: https://doi.org/10.1007/BF00732085