Kavli Affiliate: Lile Wang
| First 5 Authors: Nannan Yue, Lile Wang, Thomas Bisbas, Donghui Quan, Di Li
| Summary:
Turbulent diffuse molecular clouds can exhibit complicated morphologies
caused by the interactions among radiation, chemistry, fluids, and fields. We
performed full 3D simulations for turbulent diffuse molecular interstellar
media, featuring time-dependent non-equilibrium thermochemistry co-evolved with
magnetohydrodynamics (MHD). Simulation results exhibit the relative abundances
of key chemical species (e.g., C, CO, OH) vary by more than one order of
magnitude for the "premature" epoch of chemical evolution ($tlesssim 2times
10^5~{rm yr}$). Various simulations are also conducted to study the impacts of
physical parameters. Non-ideal MHD effects are essential in shaping the
behavior of gases, and strong magnetic fields ($sim 10~mu{rm G}$) tend to
inhibit vigorous compressions and thus reduce the fraction of warm gases
($Tgtrsim 10^2~{rm K}$). Thermodynamical and chemical conditions of the gas
are sensitive to modulation by dynamic conditions, especially the energy
injection by turbulence. Chemical features, including ionization (cosmic ray
and diffuse interstellar radiation), would not directly affect the turbulence
power spectra. Nonetheless, their effects are prominent in the distribution
profiles of temperatures and gas densities. Comprehensive observations are
necessary and useful to eliminate the degeneracies of physical parameters and
constrain the properties of diffuse molecular clouds with confidence.
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