Astron. Astrophys. 359, 780-787 (2000) 6. Numerical results for a single Lorentzian lineIn order to obtain some insight into the behavior of radiative fluxes in a medium of high optical depth according to the above equations we consider the simple case (which, however, already contains the essential features) of a continuum that does not dependent on and a single spectral line of Lorentzian shape at with damping constant (in the -scale, cf. Wehrse et al. 1998), i.e. so that In order check when the diffusion limit is reached we plot in Fig. 2 the value of the last integral in Eq. (38) as a function of s for and some values of the line strength A; the other integral behaves in the same way. It is seen that there is hardly any longer a variation for , i.e. the diffusion limit is reached for at latest. By additional line absorption it may even be shifted to much smaller values. The dependence of the monochromatic flux in the line center on the strength of the continuum and of the line A (Fig. 3) for given constant w is basically the same as in the static case: an increase in the extinction leads to a decrease in the flux independent of the source of the extinction. This implies that lines have an influence on the flux only when they are are of sufficient strength. As is seen in Fig. 4, a reduction in the velocity gradient or in the damping width leads to a decrease in the monochromatic flux at the line center. However, the main variations occur only for small and w values since for large w the line is essentially smeared out and the information on the intrinsic is lost. This behavior holds only for the monochromatic flux at or close to the line center; in contrast, for the flux integrated over the line the situation is different since in moving configurations the influence of the line extends (cf. Fig. 5) much further in wavelength than in the static case. Fig. 5 also demonstrates that for a given distance () from the line center the dependence of the flux may be quite complicated, since changes in the intrinsic line profile may or may not be compensated by Doppler shifts. Furthermore, it is seen that the line influence is - in accordance with Fig. 3 - under most conditions strongest at the line center.
© European Southern Observatory (ESO) 2000 Online publication: July 7, 2000 |