The Rosseland mean opacity of stellar atmospheres

Rosseland mean opacities $\text{a}\text{?}{}_{\mathrm{R}}\text{(T,}\text{lgP}{}_{\mathrm{e}}\text{)}$ see Table 2] per unit hydrogen particle are calculated in this paper for the atmosphere of the solar type see Table 1].The sources of the continuous opacities under consideration in this paper are as follows: (1) H^?, HI, H^?₂, H⁺₂ He^?, HeI, HeII, CI, CII, CIII, NI, NII, NIII, OI, OII, NaI, MgI, MgII, AlI, AlII, SiI, SiII, CII, KI, CaII in the form of absorption. (2) HI, HeI, CI, NI, OI, H₂ in the form of Rayleigh scattering. (3) Free electrons in the form of Thomson scattering.