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This booklet presents the main entire account to be had of basic descriptive sunlight physics. it truly is of serious worth to the meteorologist, the biologist, and the other scientist from one other self-discipline who must think of the radiations from the solar, in addition to to the layman attracted to astronomy. the pro astronomer also will locate it most fitted as a basic survey of sunlight observations. . .

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The earlier his of these classifications were influenced by the general appearance of the spectra, but later different criteria were adopted, in order to improve the accuracy of the classifications. Nevertheless, it cannot be said that the one most widely accepted today, the result of the extensive work done at Harvard College Observatory, is entirely satisfactory, since it is still necessary to solve the problem of estab- lishing well defined criteria for a classification which is based on physical principles in accordance with the theory of stellar atmospheres.

Stars is account of radiation towards that in the inner parts of the layers on at various wavelengths absorption a selective the outside. As a result its series intense, gives the most and K lines of ionized of the highest levels. The yellow D 3 line line, which 47 is the The H is also one of The Stars The Stellar intensity of the absorption lines of the photosphere is very similar to that of the lines produced by an electric arc, whilst the intensity of the emission lines of the reversing layer of the spark spectrum.

In the case of nebulae, and of stars having spectra which contain emission lines, we have to turn to other methods in order to determine the temperature. On the whole there are several ways by which we can fact they are not, since they determine the temperature of the When we physical characteristic. are referring to its which is such an important about temperature of a star, stars, talk surface temperature; to determine that of we must rely on its theoretical considerations. By means of Planck's equation, which gives the quantity of energy radiated by a black body at every wavelength, and by means of Stefan and Wien's laws which are derived from it, we can calculate the temperature of a star.

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