The spectrally resolved radiative opacity and the Rosseland and Planck mean opacities are calculated by using the detailed-term-accounting approximation for aluminum plasmas with varieties of density and temperature. The results are presented along a 40 eV isothermal sequence, a $0.01\hspace{0.5em}{\mathrm{g}/\mathrm{c}\mathrm{m}}^3$ isodense sequence, and a sequence with average ionization degree $Z*\sim \mathrm{7.13.}$ Particular attention is given to the influence of the detailed treatment of spectral lines on the Rosseland mean opacity under different thermodynamical conditions. The results show that at densities of $0.004\hspace{0.5em}{\mathrm{g}/\mathrm{c}\mathrm{m}}^3$ and higher, the opacities are not very sensitive to the spectral linewidth within a reasonable range. As examples, the Rosseland mean opacity, which is most sensitive to the detailed linewidth, at 40 eV and $0.004\hspace{0.5em}{\mathrm{g}/\mathrm{c}\mathrm{m}}^3$ changes no more than 15%, when we change the electron impact spectral linewidth artificially by reducing it by 50% or increasing it twice, and at 40 eV and $0.1\hspace{0.5em}{\mathrm{g}/\mathrm{c}\mathrm{m}}^3$ it changes less than 5%. For comparison, we also carried out calculations by using an average atom model. For the Rosseland mean opacities, the two models show quite large differences, in particular at low densities, while for the Planck mean opacities the results of the two models are much closer.

• Received 7 January 2002

DOI:https://doi.org/10.1103/PhysRevE.66.016401