By H.E. Landsberg (ed.), J. Van Mieghem (ed.)
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Additional info for Advances in Geophysics, Vol. 8
Much, if not all, of the solar corpuscular radiation probably originates in the corona. That which originates a t lower levels, say in the chromosphere, can hardly traverse the corona without exhibiting some such major effect as the whiplike phenomena observed. Since the mean free paths for nonrelativistic particles are small compared to the thickness of the corona, corpuscular clouds ejected from the chromosphere and escaping from the sun must push aside or carry along the overlying coronal gases.
The line profiles broaden considerably, and the intensities of the lines from the ions with higher ionization potentials increase relative to those from ions with lower ionization potentials. It is only in such regions that the rare yellow line of Ca XV (ionization potential -820 volts) at 5694 A is observed. The dimensions of the active regions in the corona are commonly in excess of lo6 km. The general increase in intensities of the line and continuum emission is due primarily to a density increase, which may be as much as a factor of ten in the low corona.
Speeds of motion for active region prominences generally range from 50 km/sec t o 100 km/sec, but. often reach 500 km/sec and occasionally exceed 1000 km/sec. Quiescent prominences are often of enormous size and brightness. They cannot be accurately called a phenomenon of the undisturbed sun, since thcy occur in isolated places and because they appear quite generally t,o have an association with solar active regions. Typically, thcy form on the poleward boundaries of active regions. Many drift slowly poleward as t,he region evolves and may reach large distances from their parent region.
Advances in Geophysics, Vol. 8 by H.E. Landsberg (ed.), J. Van Mieghem (ed.)