The OPAS opacity model has been used to calculate the radiative opacity of stellar plasmas in local thermodynamic equilibrium. According to the recent chemical composition revision of the solar photosphere, opacities have been computed for various hydrogen and metallic element mass fractions. Calculations have been performed toward solar interior modeling for temperatures between log[T(K)] = 6 and log[T( K)] = 7.2, and for electron densities between 10(20) and 10(26) cm(-3). We discuss possible sources of uncertainty in the calculations. We also compare Rosseland opacities to OPAL and OP data.
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