MetaData: run_name: StromgrenSphere-3D # 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: 16 time_begin: 0. # The starting time of the simulation (in internal units). time_end: 0.512 # end time 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: 0.001 # Time between snapshots # Parameters governing the conserved quantities statistics Statistics: time_first: 0. delta_time: 1e-3 # 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: 0.8 # Courant-Friedrich-Levy condition for time integration. minimal_temperature: 10 # Kelvin # Parameters related to the initial conditions InitialConditions: file_name: ./stromgrenSphere-3D.hdf5 # The file to read periodic: 1 # periodic ICs. Stars: resolution_eta: 1.2348 # (Optional) Target smoothing length in units of the mean inter-particle separation (1.2348 == 48Ngbs with the cubic spline kernel). Defaults to the SPH value. GEARRT: f_reduce_c: 0.01 # reduce the speed of light for the RT solver by multiplying c with this factor CFL_condition: 0.9 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: [1.764e+04, 3.631e+04, 8.037e+03 ] # (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: 1.00 # 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: 1 # (Optional) manually overwrite initial mass fraction of each species (using the values you set below) mass_fraction_HI: 0.999999 # (Conditional) If overwrite_initial_ionization_fractions=1, needed to set initial HI mass fractions to this value mass_fraction_HII: 1.e-6 # (Conditional) If overwrite_initial_ionization_fractions=1, needed to set initial HII mass fractions to this value mass_fraction_HeI: 0. # (Conditional) If overwrite_initial_ionization_fractions=1, needed to set initial HeI mass fractions to this value mass_fraction_HeII: 0. # (Conditional) If overwrite_initial_ionization_fractions=1, needed to set initial HeII mass fractions to this value mass_fraction_HeIII: 0. # (Conditional) If overwrite_initial_ionization_fractions=1, needed to set initial HeIII mass fractions to this value stellar_spectrum_type: 1 # Which radiation spectrum to use. 0: constant from 0 until some max frequency set by stellar_spectrum_const_max_frequency_Hz. 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. stars_max_timestep: 6.26e-5 # (Optional) restrict the maximal timestep of stars to this value (in internal units) SPHM1RT: cred: 2.99792458e3 # value of reduced speed of light for the RT solver in code unit CFL_condition: 0.1 # CFL condition for RT, independent of hydro chi: [0, 0, 0, 0] # (Optional) initial opacity in code unit for all gas particles photon_groups_Hz: [3.288e15, 5.945e15, 13.157e15] # Photon frequency group bin edges in Hz. Needs to be 1 less than the number of groups (N) requested during the configuration (--with-RT=SPHM1RT_N). Outer edges of zero and infinity are assumed. use_const_emission_rates: 1 # (Optional) use constant emission rates for stars as defined with star_emission_rates parameter star_emission_rates: [1e-32, 1.05e11, 2.16e11, 4.80e10] # (Optional) constant star emission rates (internal unit: energy/time) for each photon frequency group to use if use_constant_emission_rates is set. # = 5e48 photons/sec and BB1e5 stellar_spectrum_type: 1 # Which radiation spectrum to use. 0: constant from 0 until some max frequency set by stellar_spectrum_const_max_frequency_Hz. 1: blackbody spectrum. stars_max_timestep: 7.812500e-06 # (Optional) restrict the maximal timestep of stars to this value (in internal units). Set to negative to turn off. stellar_spectrum_blackbody_temperature_K: 1.e5 # (Conditional) if stellar_spectrum_type=1, use this temperature (in K) for the blackbody spectrum. skip_thermochemistry: 0 # (Optional) skip the thermochemistry. This is intended only for debugging and testing the radiation transport, as it breaks the purpose of RT. init_mass_fraction_metal: 0. # (Optional) Inital mass fraction of particle mass in *all* metals (if it is set, the initial fraction will be over-written.) init_mass_fraction_Hydrogen: 1.0 # (Conditional) (if init_mass_fraction_metal != -1.0f) Inital mass fraction of particle mass in Hydrogen init_mass_fraction_Helium: 0.0 # (Conditional) (if init_mass_fraction_metal != -1.0f) Inital mass fraction of particle mass in Helium coolingon: 1 # (Optional) switch for cooling (and photoheating), but photo-ionization will be ongoing even if coolingon==0 useabundances: 1 # (Optional) use the species abundances below, instead of reading from initial condition init_species_abundance_e: 1e-5 # (Conditional) (if useabundances==1) free electron abundances (in unit hydrogen number density:nH) init_species_abundance_HI: 0.99999 # (Conditional) (if useabundances==1) HI abundances (in unit hydrogen number density:nH) init_species_abundance_HII: 1e-5 # (Conditional) (if useabundances==1) HII abundances (in unit hydrogen number density:nH) init_species_abundance_HeI: 0.0 # (Conditional) (if useabundances==1) HeI abundances (in unit hydrogen number density:nH) init_species_abundance_HeII: 0.0 # (Conditional) (if useabundances==1) HeII abundances (in unit hydrogen number density:nH) init_species_abundance_HeIII: 0.0 # (Conditional) (if useabundances==1) HeIII abundances (in unit hydrogen number density:nH) relativeTolerance: 1e-3 # (Optional) Relative tolerance for SPHM1RT thermo-chemistry intergration absoluteTolerance: 1e-10 # (Optional) Absolute tolerance for SPHM1RT thermo-chemistry integration explicitTolerance: 0.1 # (Optional) Tolerance below which we use the explicit solution in SPHM1RT thermo-chemistry ionizing_photon_energy_erg: [3.0208e-11, 5.61973e-11, 1.05154e-10] # (Optional) ionizing photon energy in erg averaged within frequency bins