Astronomy and Astrophysics – Astronomy
Scientific paper
Mar 1978
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...220..643r&link_type=abstract
Astrophysical Journal, Part 1, vol. 220, Mar. 1, 1978, p. 643-645, 647, 649-653, 655-665. Research supported by the Smithsonian
Astronomy and Astrophysics
Astronomy
1025
Solar Activity, Solar Corona, Solar X-Rays, X Ray Astronomy, Astronomical Models, Convective Flow, Hydrostatic Pressure, Parameterization, Plasma Control, Skylab Program, Stellar Magnetic Fields
Scientific paper
An analytical model for the quiescent inhomogeneous solar corona is developed on the basis of the hypothesis that looplike structures are the basic coronal building blocks. By assuming that quiescent loop structures observed in X-rays are in hydrostatic equilibrium, it is demonstrated that such loops must have their temperature maximum located near their apex and that substantial nonradiative energy deposition must occur along most of their length. The calculations yield a unique relation among loop temperature, pressure, and size, which fits the X-ray observations of quiescent structures well and is consistent with the initial assumption of hydrostatic equilibrium. The results suggest that the coronal loops visible in X-rays represent a relatively steady-state equilibrium of the confined plasmas and that fluctuations in such quantities as the local heating rate can lead to dynamically unstable states in which the loop plasma does not attain a temperature sufficient for X-ray emission. A parameterization of various proposed coronal heating theories is also developed within the context of the analytical model.
Rosner Robert
Tucker Wallace H.
Vaiana Giuseppe S.
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