Abstract:
Turbulence features ubiquitously in the interstellar medium, especially in the high-redshift Universe. Photoionization models with turbulent ISM density fields can predict nebular emission lines more realistically than the former uniform density/pressure photoionization models. In this talk, we will briefly introduce a turbulent photoionization model grid created by the cutting-edge 3D Monte Carlo MAPPINGS code (M3). This grid is built on turbulence-like ISM density fields with log-normal density distributions and the Kolmogorov power spectrum. We will present the dependence of the nebular emission-line ratios on the ISM turbulent structures. This work provides a theoretical support for understanding the high-redshift emission-line galaxies observed by JWST.
