On the effect of temperature fluctuations on line intensities

Details On the effect of temperature fluctuations on line intensities On the effect of temperature fluctuations on line intensities

Sep 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983jqsrt..30..193g&link_type=abstract

Journal of Quantitative Spectroscopy and Radiative Transfer (ISSN 0022-4073), vol. 30, Sept. 1983, p. 193-211.

Statistics

Computation

4

Line Spectra, Stellar Atmospheres, Stellar Spectra, Temperature Effects, Atmospheric Temperature, Atomic Excitations, Electron Transitions, Radiative Transfer

Scientific paper

The effects of temperature fluctuations in a stellar atmosphere on the intensities of the lines emitted by a multilevel atom are investigated by differentiating the coupled set of radiative transfer and statistical equilibrium equations. A numerical method is proposed for the fast computation of large sequences of line profiles when the atmospheric temperatures are fluctuating about a mean curve T(z) (oscillations, waves, turbulence, etc.) This method is applied to a three-level atom simulating the formation of Ca(II) lines in the solar atmosphere and the results are compared with those of direct computations. It is shown how the variations of atomic level populations, line source functions, and emergent intensities may be related to temperature variations by a sum of several terms corresponding to each atomic transition and arising from the variations of collisional excitation rates. Finally, the possibility of extending the method to compute profile variations when temperatures, densities and velocities are changing simultaneously within the atmosphere is discussed.

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