By H.E. Landsberg (ed.), J. Van Mieghem (ed.)
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Additional resources for Advances in Geophysics, Vol. 8
ATHAY AND C. S. WARWICK ment of the emission from ions with high ionization potential and the widening of the line profile both suggest higher temperatures in these active regions than in normal coronal regions. The increased density and emission diminish in both the outward radial and tangential directions, and in a rough sort of way the coronal region can be visualized as a localized condensation of increased density and temperature in the lower corona. Indications are that the temperature may reach 3-5 X 1Oe0K.
Forbidden lines appear in t,he coronal spectjrum, in opposition to normal laborat,ory spec,t,ra,because of t>hecombination of high kinetic temperature and low elcct,roii density. es t,o their value as probes of coronal activity. The same ions which produce these lines must also radiate in the far ultraviolct, and x-ray spec,trum wit,h much greater intensity than in t8hefuiiit forbidden lines. ronger permitted lines. ed in t,he same wavelength interval from a blackbody a t 2 X 1O6"K 71. Two problems of long-standing interest in the corona arc: (1) tJhe source of energy for producing the high kinct,ic temperature, and ( 2 ) the explanation for the highly irregular geometry.
The chief characteristic of type I1 (slow drift) and type I11 (fast drift) bursts is the drift of the emission toward lower frequency with time. This drift can be explained as due to a source moving outward through the corona, emitting a t the plasma frequency, which decreases as the electron density decreases. 16. Schematic representation of radio bursts following a large solar flare. 48 R. G. ATHAY AND C. S. WARWICK relation in a coronal streamer, and that the emission at a given height is essentially monochromatic.