By Leo Goldberg, A. Keith Pierce (auth.), S. Flügge (eds.)
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Additional resources for Astrophyysics III: The Solar System / Astrophysik III: Das Sonnensystem
No. 43 (1954). R. LUNDBLAD: Astrophys. J ourn. 58, 113 (1923). (17·3) 25 The continuous absorption coefficient. Sect. 17. in which e(x) and d x/dT are constant for a given temperature, T, corresponding to a fixed depth in the atmosphere. , is derivable from observation, while k;. of the right member may be obtained from quantum mechanical calculation, or from laboratory measurements. Hence one should have an excellent check on all phases of the problem. i;. ) = a;. + ;. 000 a b Fig. 11 a and b.
VITENSE: Z. Astrophys. 34, 209 (1954). 32 Sect. 20. LEO GOLDBERG and A. KEITH PIERCE: The Photosphere of the Sun. members of the Balmer series and the cores of the strongest iron lines are formed in the lower part of the chromosphere and are strongly affected by temperature inhomogeneities (Sect. 40). Furthermore, the temperature found from central intensities of strong Fraunhofer lines represent excitation temperatures of the upper levels of the transition and because of departure from thermodynamic equilibrium cannot be identified with the boundary temperature derived from the continuum.
0. 1. pable of absorbing in these continua. For example, for the ratio of the number Fig. 10. The optical depth as a function of wavelength for f . h various fixed depths in the solar atmosphere defined by 0 atoms In t e third quantum level capable of absorbing the Paschen conf} = 5040 T . jNH = 6 X 10-10 , for T = 6000°. However, this number rises very quickly in the deeper layers and the H- ion gradually loses out. The absorption coefficient of H may be found in the tables of UNSOLD [1J or in the work of UENO, SAITO, and ]UGAKU2.
Astrophyysics III: The Solar System / Astrophysik III: Das Sonnensystem by Leo Goldberg, A. Keith Pierce (auth.), S. Flügge (eds.)