  Massive, young stars are the main source of energy that maintains multiphase
structure and turbulence in the interstellar medium (ISM), and without this
"feedback" the star formation rate (SFR) would be much higher than is observed.
Rapid energy loss in the ISM and efficient energy recovery by stellar feedback
lead to co-regulation of SFRs and the ISM state. Realistic approaches to this
problem should solve the dynamical evolution of the ISM, including star
formation, and the input of feedback energy self-consistently and accurately.
Here, we present the TIGRESS-NCR numerical framework, in which UV radiation,
supernovae, cooling and heating processes, and gravitational collapse are
modeled explicitly. We use an adaptive ray tracing method for UV radiation
transfer from star clusters represented by sink particles, accounting for
attenuation by dust and gas. We solve photon-driven chemical equations to
determine the abundances of H (time-dependent) and C/O-bearing species
(steady-state), which then set cooling and heating rates self-consistently.
Applying these methods, we present high-resolution magnetohydrodynamics
simulations of differentially rotating local galactic disks representing
typical conditions of nearby star-forming galaxies. We analyze ISM properties
and phase distributions and show good agreement with existing multiwavelength
galactic observations. We measure midplane pressure components (turbulent,
thermal, and magnetic) and the weight, demonstrating that vertical dynamical
equilibrium holds. We quantify the ratios of pressure components to the SFR
surface density, which we call the feedback yields. The TIGRESS-NCR framework
will allow for a wide range of parameter exploration, including low metallicity
system.
