The results of measurements of absolute intensities in the spectrum of the centre of the sun's disk in the wavelength region 2977-4087/~ have already been published (Houtgast 1965(Houtgast , 1968 and use has been made of them on different occasions. The intensities at 206 spectral points have been given, chosen as much as possible between the Fraunhofer lines, but well divided over the region. Each strip of the Utrecht (Minnaert et al., 1940) and G~Sttingen (BriJckner, 1960) Atlases contains at least two points. Later (Houtgast and Namba, 1968) four more points were added below 2 2977/~.In order to judge the reliability of the published intensities one requires a description of the observational method. This description includes the apparatus, the correction for atmospheric extinction and the number of observations from which the final mean values of the absolute intensities are deduced. Finally a discussion of the most important sources of error is given.
We present results from eclipse spectra in the wavelength region 4588-4682 A., taken during the eclipse of February 15, 1961 at Bra6, Yugoslavia. Absolute line intensities have been determined in the photosphere-chromosphere transition region. The method of reduction is discussed in Section 2 and the observed variation of the total intensity as a function of the height is shown for a number of lines in Figures 5-8. The results for the Fe I lines are compared with computations (as described in Paper I: van Dessel, 1970) for various solar model atmospheres (Section 4). The model, which combines Holweger's (1967) temperature distribution for the excitation temperature with the HSRA model (Gingerich et al., 1971) for the electron temperature, yields a better agreement than all pure LTE-models. Solar Physics 33 (1973) 375-391. All Rights Reserved Coovri~ht ~ 1973 bv D. Reidel Publishine Comnanv. Dordreeht-Hollancl
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