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Closed coronal structures. II - Generalized hydrostatic model
Serio, S.; Peres, G.; Vaiana, G. S.; Golub, L.; Rosner, R.
AA(Harvard-Smithsonian Center for Astrophysics, Cambridge, Mass; Osservatorio Astronomico, Palermo, Italy), AB(Harvard-Smithsonian Center for Astrophysics, Cambridge, Mass; Osservatorio Astronomico, Palermo, Italy), AC(Harvard-Smithsonian Center for Astrophysics, Cambridge, Mass; Osservatorio Astronomico, Palermo, Italy), AD(Harvard-Smithsonian Center for Astrophysics, Cambridge, Mass.), AE(Harvard-Smithsonian Center for Astrophysics, Cambridge, Mass.)
Astrophysical Journal, Part 1, vol. 243, Jan. 1, 1981, p. 288-300. Research supported by the Smithsonian Institution, Consiglio Nazionale delle Ricerche, and CRRN; (ApJ Homepage)
Publication Date:
Solar Physics
NASA/STI Keywords:
Atmospheric Models, Coronal Holes, Coronal Loops, Magnetohydrostatics, Solar Atmosphere, Solar Corona, Atmospheric Heating, Base Pressure, Magnetohydrodynamics, Solar Physics, Solar Prominences, Temperature Distribution, Temperature Inversions
Bibliographic Code:


Numerical computations of stationary solar coronal loop atmospheres are used to extend earlier analytical work. Two classes of loops are examined, namely symmetric loops with a temperature maximum at the top but now having a length greater than the pressure scale height and loops which have a local temperature minimum at the top. For the first class, new scaling laws are found which relate the base pressure and loop length to the base heating, the heating deposition scale height, and the pressure scale height. It is found that loops for which the length is greater than about two to three times the pressure scale height do not have stable solutions unless they have a temperature minimum at the top. Computed models with a temperature inversion at the top are permitted in a wider range of heating deposition scale height values than are loops with a temperature maximum at the top. These results are discussed in relation to observations showing a dependence of prominence formation and stability on the state of evolution of magnetic structures, and a general scenario is suggested for the understanding of loop evolution from emergence in active regions through the large-scale structure phase to opening in coronal holes.

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