Radiative Excitation, Ionization, Recombination, and Fluorescence
Part of the Astrophysics and Space Science Library book series (ASSL, volume 112)
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Before we can calculate rate processes for atomic events in gaseous nebulae, we must derive certain basic equations. Our first concern is with radiative processes involving hydrogen.
KeywordsCharge Exchange Solar Corona Central Star Planetary Nebula Ground Term
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- Our discussion of absorption and emission processes involving H is taken from D.H. Menzel, 1937, Ap. J., 85, 330. This and other papers of the Harvard series on physical processes in gaseous nebulae are reprinted in: Physical Processes in Ionized Plasmas, ed. D.H. Menzel (New York: Dover Publications, 1962, hereafter referred to as PPIP).ADSzbMATHCrossRefGoogle Scholar
- Hydrogenic line and continuous absorption coefficients have been discussed by: Burgess, A. 1964, M.N.R.A.S., 69, 1.Google Scholar
- For a discussion of continuous absorption coefficients for complex atoms see: Burke, P.G. Atomic Processes and Applications, ed. P.G. Burke and B.L. Moiseiwitsch (Amsterdam: North-Holland Publications, 1976).Google Scholar
- The cross sections given by these authors for dielectronic recombination appear to be systematically too small. Dielectronic Recombination. A general review with references to previous work is given by: Seaton, M.J., and Storey, P.G. Atomic Processes and Applications, ed. P.G. Burke and B.L. Moiseiwitsch (Amsterdam: North-Holland Publications, 1976, p. 134).Google Scholar
- Dielectronic recombination rates appropriate to nebular temperatures and densities are discussed, for example, by: Nussbaumer, H., and Storey, P.J. 1983, Astron. Astrophys.Google Scholar
- Charge Exchange. A brief summarizing account of the problems of charge exchange, with references to earlier work and timely warnings pertaining to inherent uncertainties in theoretical calculations, is given by: Dalgamo, A. Planetary Nebulae (ed. Y. Terzian, International Astronomical Union Symposium No. 76, Dordrecht, Reidel, 1978, p. 139).Google Scholar
- A summary of the earlier work with descriptions of investigations by: Ambarzumian (1932), Stoy (1933), Wurm (1951), and others are given by: Aller, L.H., and Liller, W. 1968, Stars and Stellar Systems, 7, 546Google Scholar
- A summary of the earlier work with descriptions of investigations by: Ambarzumian (1932), Stoy (1933), Wurm (1951), and others are given by: Aller, L.H., and Liller, W. 1968, Nebulae and Interstellar Matter, ed. by Barbara Middlehurst and L.H. Aller, Chicago, Univ. Chicago Press.Google Scholar
- Bowen proposed his fluorescent mechanism in: 1935, Ap. J., 81, 1. The earliest theoretical treatments by D.H. Menzel and L.H. Aller, 1941, Ap. J., 94, 436Google Scholar
- T. Hatanaka, 1947, J. Astr. Geophys. Japan, 21, 1Google Scholar
- T. Kallman and R. McCray, 1980, Ap. J., 242, 615, discuss its possible importance in X-ray sources where much of the soft X-ray luminosity absorbed by the nebula appears as Lya (He II) which controls the ionization and temperature structure of the plasma until degraded. The BFM is expected to have a major effect on the fate of these He II photons.ADSCrossRefGoogle Scholar
© D. Reidel Publishing Company, Dordrecht, Holland 1984