Abstract
This chapter gives a review of spectral line formation processes, starting with the main equations valid in thermodynamic equilibrium. The Einstein coefficients and the main spectral line profile functions are discussed.
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Drake, G.W.F.: Atomic, Molecular and Optical Physics Handbook. American Institute of Physics, New York (1996). Includes detailed tables of atomic and molecular data
Finn, G.D., Mugglestone, D.: Mon. Notices Roy. Tables of the line broadening function H(a,v). Astron. Soc. 129, 221 (1965). Tables of the line broadening function H(a,v). Includes tables for the Hjerting function under several conditions. Other tabulations may be found in Harris, D.L. 1948. Astrophys. J. 108:112; and Hjerting, F. 1938. Astrophys. J. 88:508
Jefferies, J.T.: Spectral Line Formation. Blaisdell, Waltham (1968). Complete treatment of spectral line formation in astrophysical conditions and broadening processes
Lang, K.R.: Astrophysical Formulae. Springer, Berlin (1999). Referred to in Chapter 2. Includes basic equations of TE, Einstein coefficients definitions, and references to original works
Maciel, W.J.: Introdução à Estrutura e Evolução Estelar. Edusp, São Paulo (1999). Introduction to stellar structure and evolution, including a discussion on the main radiation field concepts, such as intensity and flux
Mihalas, D.: Stellar Atmospheres. W.H. Freeman, San Francisco (1978). Discussion on radiative transfer in stellar atmospheres and spectral line profiles. Includes problems related to line formation in atmospheres and expanding envelopes
Morton, D.C., Dinerstein, H.L.: Astrophys. J. 204, 1 (1976). Tables with oscillator strength values for lines of astrophysical interest. See also Astrophys. J. Suppl. vol. 26, p.333, 1973
Reif, F.: Fundamentals of Statistical and Thermal Physics. McGraw-Hill, New York (1965). Basic text of thermodynamics and statistical physics, including a good discussion of TE equations
Rybicki, G.B., Lightman, A.P.: Radiative Processes in Astrophysics. Wiley, New York (1979). Referred to in Chapter 2. Good discussion of TE equations, absorption and emission coefficients, and radiative transfer
Shu, F.H.: The Physics of Astrophysics, vol. 1. University Science Books, Mill Valley (1991). Advanced treatment of radiative transfer with astrophysical applications
Unsöld, A.: Physik der Sternatmosphären. Springer, Berlin (1955). Classical text on stellar atmospheres, with a good discussion of spectral line formation in stars and of the Voigt profile
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Exercises
Exercises
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3.1
Show that the free electrons partition function per unit volume is given by relation (3.14).
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3.2
Show that the Doppler profile (3.48) is normalized.
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3.3
Show that the Lorentz profile (3.50) is normalized and that in this case the FWHM is Δν h = Γ k /2π.
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3.4
Collisional processes, radiation absorption, recaptures from the continuum, etc., maintain the population of 108 atoms at a certain energy level k. The Einstein emission coefficient relative to a lower level j is A kj ≃ 108 s−1. (a) What is the number of spontaneous emissions per second for level j? (b) What is the radiative lifetime of level k relatively to emissions to level j?
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3.5
Calculate the oscillator strengths f jk and f kj for the neutral H 21 cm line, which has an emission coefficient A kj ≃ 2.9 × 10−15 s−1.
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Maciel, W.J. (2013). Spectral Line Formation. In: Astrophysics of the Interstellar Medium. Springer, New York, NY. https://doi.org/10.1007/978-1-4614-3767-3_3
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DOI: https://doi.org/10.1007/978-1-4614-3767-3_3
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