Modelo de angstrom e análise dos componentes atmosféricos que atenuam a radiação solar

Abstract

Of the total energy irradiated by the sun, only a very small part is interpreted by the terrestrial globe. Of this large amount mentioned above, only 2.0 cal / mincm3 reaches the top of the atmosphere on average and is called the solar constant. To explain this prodigious energy, which reached the earth at least five billion years ago, numerous hypotheses were put forward, but until 1938 none of them had been able to explain the phenomenon in a convincing way. The problem began to be taken very seriously, from the moment that there is a need to harness energy from solar sources. The use of solar energy necessarily requires detailed knowledge of the characteristics of the incidence of solar radiation on the surface of the globe. Because, energy entering the atmosphere undergoes absorption, reflection and diffusion phenomena due to air molecules, particles suspended in the atmosphere, water vapor, ozone and other constituents of the atmosphere. On the other hand, in the professional activity of engineers, architects, agronomists and others, problems often arise that can only be solved conveniently by knowing the temporal and spatial availability of solar energy.