ATOMIC CHEMISTRY IN TURBULENT ASTROPHYSICAL MEDIA. II. EFFECT OF THE REDSHIFT ZERO METAGALACTIC BACKGROUND

Abstract

ABSTRACT We carry out direct numerical simulations of turbulent astrophysical media exposed to the redshift zero metagalactic background. The simulations assume solar composition and explicitly track ionizations, recombinations, and ion-by-ion radiative cooling for hydrogen, helium, carbon, nitrogen, oxygen, neon, sodium, magnesium, silicon, sulfur, calcium, and iron. Each run reaches a global steady state that depends not only on the ionization parameter, U , ?> and mass-weighted average temperature, T MW , ?> but also on the one-dimensional turbulent velocity dispersion, &sgr; 1D ?> . We carry out runs that span a grid of models with U ranging from 0 to 10−1 and &sgr; 1D ?> ranging from 3.5 to 58 km s−1, and we vary the product of the mean density and the driving scale of the turbulence, nL , ?> which determines the average temperature of the medium, from nL = 10 16 ?> to nL = 10 20 ?> cm−2. The turbulent Mach numbers of our simulations vary from M ≈ 0.5 ?> for the lowest velocity dispersion cases to M ≈ 20 ?> for the largest velocity dispersion cases. When M ≲ 1 , ?> turbulent effects are minimal, and the species abundances are reasonably described as those of a uniform photoionized medium at a fixed temperature. On the other hand, when M ≳ 1 , ?> dynamical simulations such as the ones carried out here are required to accurately predict the species abundances. We gather our results into a set of tables to allow future redshift zero studies of the intergalactic medium to account for turbulent effects.