Physics
Scientific paper
May 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986soph..105...51f&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 105, May 1986, p. 51-65.
Physics
2
Chromosphere, Coronal Loops, Solar Activity, Solar Magnetic Field, H Alpha Line, Magnetic Field Configurations, Maps, Photosphere, Potassium, Solar Flares, Velocity Distribution
Scientific paper
Based on 54 maps obtained at the Paris-Meudon Observatory, the emissive features detected in nine active regions (ARs) and observed on the disk at different levels of the chromosphere are studied, and 11 archshaped structures have been detected which may be interpreted as stable loops. The footpoints are located on both sides of an inversion region in the magnetic field, and it is suggested that the magnetic lines of force may have an oblique direction relative to the solar surface. The mean distance between the feet of the arches is about 30,000 km, with arch heights lower in the young AR, higher when it evolves, and scarcely detectable when the Ar is dying. The maximum peaks in the blue wing of the K line are noted at the periphery of the highest H-alpha and K3 intensity values or at the periphery of the AR, and observations of unstable loops during flares suggest a characteristic relationship between the stable loop and the transient flaring loop consisting of the flaring arch having one of its footpoints in common with a closer stable, preexisting arch at the maximum of the flares.
Fang Chen
Martres Marie-Josephe
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