Astrophyysics III: The Solar System / Astrophysik III: Das by Leo Goldberg, A. Keith Pierce (auth.), S. Flügge (eds.)

By Leo Goldberg, A. Keith Pierce (auth.), S. Flügge (eds.)

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Extra resources for Astrophyysics III: The Solar System / Astrophysik III: Das Sonnensystem

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Soc. Amer. 47, 6 (1957). R. McMATH: Astrophys. Journ. 123, 1 (1956). Observatory _76, 241 Sect. 22. 37 Wavelengths. , and the location of the windows is shown in Fig. 15. The ultraviolet limit for ground observation is about A 2935, but the radiation spectrum at shorter wavelengths has been observed from rockets to wavelengths as short as 1 to 2 A. However, the photospheric or Fraunhofer spectrum has really been observed only to about A 1600. The reason is that, at shorter wavelengths, the intensity of the continuous spectrum is too weak to be well observed in the exposure times possible with rockets, and hence only the line emission from the chromosphere and corona has been so recorded.

The special significance of these numbers is that the true half-widths of faint Fraunhofer lines are about three times greater than the instrumental half-widths and therefore the profiles of the weak lines may be directly observed. 7% of the continuum at A. 8 %. In the cores of the Hand K lines the total contribution of scattering and ghosts is no more than about 2 % according to a recent unpublished determination by MOHLER. Thus, the fact that both the profiles and the absolute central intensities of weak as well as strong lines may now be observed with relatively high precision presages a period of intensive re-analysis of the Fraunhofer spectrum in which heavy emphasis will be laid on the detailed elucidation of the photospheric structure from individual line profiles.

Abundance investigations will continue to be based on the equivalent widths of weak lines, which can now be measured with much higher accuracy than heretofore. It should be remarked, however, that the problems of establishing the position of the continuum and of correcting for blending still deserve the most careful observational and theoretical attention. In the succeeding sections, we shall first refer briefly to the observational data upon which investigations of the Fraunhofer spectrum are based, then sketch the theory of Fraunhofer-line formation, and finally review some of the more recent analytic studies of the spectrum.

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