Closed coronal structures. III - Comparison of static models with X-ray, EUV, and radio observations

Details Closed coronal structures. III - Comparison of static models with X-ray, EUV, and radio observations Closed coronal structures. III - Comparison of static models with X-ray, EUV, and radio observations

Jul 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...247..692p&link_type=abstract

Astrophysical Journal, Part 1, vol. 247, July 15, 1981, p. 692-706. Research supported by the Smithsonian Institution and Consi

Astronomy and Astrophysics

Astronomy

66

Coronal Loops, Solar Corona, Solar X-Rays, Stellar Models, X Ray Astronomy, Centimeter Waves, Energy Transfer, Extreme Ultraviolet Radiation, Scale Height, Scaling Laws, Skylab Program, Solar Activity Effects, Solar Atmosphere, Solar Radiation, Solar Radio Emission, Stellar Evolution, Sunspots

Scientific paper

Numerical models of static coronal loops in energy balance are compared with high spatial resolution observations of extreme ultraviolet lines, broad-band X-ray emission, and interferometric observations at 2.8 cm of a solar active region. Difficulties of using scaling laws to test static models of coronal loops are reviewed. The theoretical model used for the comparison is summarized; the detailed X-ray, EUV, and microwave observations of the selected active region are presented; and the comparison of the model with the observations is performed. It is shown that simple static models with conductive flux vanishing at the loop base reproduce satisfactorily the observed properties in the upper portion of loop structures from compact, high-pressure loops in the core of the region to more extended, fainter loops and to large-scale loops interconnecting different active regions. Effects of changing loop parameters are investigated, and it is argued, that in contrast to the present approach, scaling laws cannot be used to discriminate between different static energy balance models. Some discrepancy is found between model predictions and observations for the lower sections of loop structures. Possible causes of the discrepancy are discussed.

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