MetaData: run_name: advect_ions # Define the system of units to use internally. InternalUnitSystem: UnitMass_in_cgs: 1.98841586e+33 # 1 M_Sol UnitLength_in_cgs: 3.08567758e21 # kpc in cm UnitVelocity_in_cgs: 1.e5 # km/s UnitCurrent_in_cgs: 1. UnitTemp_in_cgs: 1. # K # Parameters governing the time integration TimeIntegration: max_nr_rt_subcycles: 1 time_begin: 0. # The starting time of the simulation (in internal units). time_end: 1 # end time: radiation reaches edge of box dt_min: 1.e-12 # The minimal time-step size of the simulation (in internal units). dt_max: 1.e-03 # The maximal time-step size of the simulation (in internal units). # Parameters governing the snapshots Snapshots: basename: output # Common part of the name of output files time_first: 0. # Time of the first output (in internal units) delta_time: 0.1 # Time between snapshots # Parameters governing the conserved quantities statistics Statistics: time_first: 0. delta_time: 5e-4 # Time between statistics output # Parameters for the hydrodynamics scheme SPH: resolution_eta: 1.2348 # Target smoothing length in units of the mean inter-particle separation (1.2348 == 48Ngbs with the cubic spline kernel). CFL_condition: 0.9 # Courant-Friedrich-Levy condition for time integration. minimal_temperature: 10. # Kelvin # Parameters related to the initial conditions InitialConditions: file_name: ./advect_ions.hdf5 # The file to read periodic: 1 # periodic ICs. Keep them periodic so we don't loose photon energy. GEARRT: f_reduce_c: 1.e-5 # reduce the speed of light for the RT solver by multiplying c with this factor CFL_condition: 0.9 f_limit_cooling_time: 0.0 # (Optional) multiply the cooling time by this factor when estimating maximal next time step. Set to 0.0 to turn computation of cooling time off. photon_groups_Hz: [3.288e15, 5.945e15, 13.157e15] # Lower photon frequency group bin edges in Hz. Needs to have exactly N elements, where N is the configured number of bins --with-RT=GEAR_N stellar_luminosity_model: const # Which model to use to determine the stellar luminosities. const_stellar_luminosities_LSol: [0., 0., 0.] # (Conditional) constant star luminosities for each photon frequency group to use if stellar_luminosity_model:const is set, in units of Solar Luminosity. hydrogen_mass_fraction: 0.76 # total hydrogen (H + H+) mass fraction in the metal-free portion of the gas set_equilibrium_initial_ionization_mass_fractions: 0 # (Optional) set the initial ionization fractions depending on gas temperature assuming ionization equilibrium. set_initial_ionization_mass_fractions: 0 # (Optional) manually overwrite initial mass fraction of each species (using the values you set below) stellar_spectrum_type: 1 # Which radiation spectrum to use. 0: constant over all frequencies. 1: blackbody spectrum. stellar_spectrum_blackbody_temperature_K: 1.e5 # (Conditional) if stellar_spectrum_type=1, use this temperature (in K) for the blackbody spectrum. skip_thermochemistry: 1