Abstract The solar corona is the region of transfer, transformation, accumulation and release of “nonthermal” energy generated in the subphotospheric levels. These processes are essentially connected with the plasma structures observed in the corona. Radio astronomy methods present an unique opportunity for measuring magnetic fields, particle acceleration, plasma turbulence in the corona as well as such parameters as electron density and temperature accessible also to other techniques. To be effective radio observations need a combination of high spatial resolution with good spectral coverage and accurate polarization measurements as well as plenty of observational time. No one of the existing systems meet all these demands. However, such structures as radio granulation, coronal holes, filaments and their cavities have been studied using such instruments as VLA, WSRT and RATAN-600. Local sources of active regions prove to be very complicated structures due to a number of different mechanisms of generation of the radio emission. Using the radio telescope RATAN-600 a new type of structure - peculiar sources have been found in centimeter wavelength range. They give evidence of stable ( lasting several days ) localized regions of energy release in the lower corona. The mechanism of generation of the radio emission of these peculiar sources as well as of a decimetric halo is still in the stage of discussion. Significant progress is expected as a result of current modificationsof the RATAN-600 solar program. Cooperative programs of ground-based radio and optical observations of plasma structures of the inner corona in combination with space observations in EUV and X-rays are most prominent in resolving the problems above.
Inner corona from solar radio observations
Advances in Space Research ; 11 , 1 ; 89-97
1991-01-01
9 pages
Aufsatz (Zeitschrift)
Elektronische Ressource
Englisch
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