Physics
Scientific paper
Mar 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991soph..132...95m&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 132, March 1991, p. 95-108. Research supported by NASA and NSF.
Physics
19
Chromosphere, Coronal Loops, Energy Transfer, Solar Corona, Thermal Stability, Boundary Conditions, Digital Simulation, Solar Temperature
Scientific paper
The radiative stability of thermally isolated coronal loops with free-flow boundary conditions by nonlinear numerical simulation are studied. A chromosphere-to-corona loop equilibrium (including the option of a deep chromosphere) is first established by following the nonlinear evolution from an initial isothermal state with rigid boundaries. The end conditions are then changed, to allow free flow and to fix the temperature, and investigate the response to nonisobaric perturbations. Within a family of loops of the same pressure, long hot loops to be stable and short cool loops to be unstable to the thermal chromospheric-expansion mode are found. The stable cases remain so, even when long chromospheric ends and/or gravity are added. In those cases which are unstable, the subsequent nonlinear evolution which exhibits swelling of the chromosphere until the entire loop becomes cool and dense are followed.
Mok Yung
Schnack Dalton D.
van Hoven Gerard
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