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The process of mastering the SSRT
has been accompanied by an expansion of the
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scientific
interests and a change of the requirements to its characteristics. The
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advent
of new technologies and instrumentation made it possible to embark on the
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modernization
of the SSRT systems. The use of SHF amplifiers with a noise
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temperature
of 50 degrees allowed the SSRT sensitivity to be improved
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considerably,
enabling the recording and study of low-contrast features in the solar
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corona:
coronal holes, filament, and bright coronal points. The receiving-recording
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system
is being improved through the use of acoustooptic facilities. The
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methodology
of improving the solar corona radio image quality is under
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development.
It has been possible to achieve a spatial and temporal resolution of up
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to 15 sec of
arc and up to 14 ms, respectively.
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The relatively high angular and,
especially, temporal resolution of the SSRT,
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together
with the adequate sensitivity, made it possible to considerably extend our
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research
to almost all forms of solar activity: new models were proposed (and the
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old
models refined) for active regions, flares, formation and acceleration of
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energetic
particle fluxes, coronal mass ejections, and coronal holes. First and
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foremost
the spatial-temporal characteristics of the origination and development of
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active
regions were studied. A detailed study was made of the phenomenon of the
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sign
reversal of the circular polarization of emission from the active region
during
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its
solar disk passage, a number of new flare buildup signatures were
identified, an
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effective
criterion of flare ‘protonicity’ from the character of emission
polarization
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distribution
of the active region was developed, we studied the properties and
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