Line Formation in Turbulent Media
Since 1934, when Struve and Elvey introduced the concept of microturbulence for spectral line broadening in addition to pressure and thermal Doppler broadening, this mechanism has frequently been used in the analysis of stellar spectra. According to the discussions in standard textbooks on stellar spectra the effect of microturbulence is due to an increase in the width of the Doppler core of the line absorption coefficient with the result that the total intensities (equivalent widths) of the Fraunhofer lines at which saturation effects occur are also enhanced. Thus the flat part of the curve of growth is raised.
KeywordsRadiative Transfer Line Profile Transfer Equation Equivalent Width Turbulent Velocity
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- Batchelor, G.K.: The Theory of Homogeneous Turbulence. Cambridge: Cambridge University Press 1967.Google Scholar
- Gail, H.P., Sedlmayr, E., Traving, G.: to be published (1975).Google Scholar
- Hinze, J.P.: Turbulence. New York, Toronto, London: McGraw-Hill 1959.Google Scholar
- Pecker, J.-C., Thomas, R.N.: In: Aerodynamic Phenomena in Stellar Atmospheres IAU Symp. No 12 p.1 (ed. R.N. Thomas), Bologna 1961.Google Scholar
- Sobolev, V.V.: Moving Envelopes of Stars. Cambridge, Mass.: Harvard University Press 1960.Google Scholar