Abstract
Solar radio emission has been providing information about the Sun for over half a century. In order to fully exploit this information, one needs to have a broader view of the solar atmosphere, which cannot be provided by radio observations alone. The purpose of this review is to present this background information, which is necessary to understand the physical processes that determine the solar radio emission and to link the radio domain with the rest of the electromagnetic spectrum.
Highlights
By definition, the atmosphere of a star is the region from which photons can escape and reach the observer
The bulk of what we know about the Sun comes from photons, in this review we will restrict ourselves to the results obtained from the analysis of the solar electromagnetic emission, in an attempt to compile a concise, but still comprehensive picture of the structure of the solar atmosphere; we will try to give a historical perspective, as far as possible
Until a few decades ago, we had no direct information about the interior of the Sun; what we knew was based on the theory of stellar structure, which produced the so called standard model of the solar interior
Summary
The atmosphere of a star is the region from which photons can escape and reach the observer. As far as the time scale is concerned, solar phenomena are divided in three groups: the Quiet Sun (QS), the slowly varying component and the sporadic component. This grouping reflects the energy associated with the phenomena, with the sporadic emission being the most energetic. It is important to stress that, as the solar emission extends over a wide spectral range, from γ -rays to radio waves, no single spectral window can provide complete information on solar phenomena. We will pass to active regions and we will finish with a discussion of the heating problem
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