/******************************************************************************* * This file is part of SWIFT. * Copyright (c) 2016 Matthieu Schaller (matthieu.schaller@durham.ac.uk) * * This program is free software: you can redistribute it and/or modify * it under the terms of the GNU Lesser General Public License as published * by the Free Software Foundation, either version 3 of the License, or * (at your option) any later version. * * This program is distributed in the hope that it will be useful, * but WITHOUT ANY WARRANTY; without even the implied warranty of * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the * GNU General Public License for more details. * * You should have received a copy of the GNU Lesser General Public License * along with this program. If not, see . * ******************************************************************************/ #ifndef SWIFT_DUST_CONSTANTS_H #define SWIFT_DUST_CONSTANTS_H /* Config parameters. */ #include /* Dust-to-gas ratio representing the solar neighbourhood, matching value * assumed internally by CHIMES.*/ static const float local_dust_to_gas_ratio = 0.006; /* Solar metallicity following Wiersma (2009a) enrichment tables */ static const float solar_metallicity_wiersma = 0.0127; /* Typical grain radius in cm, consistent with AGB and SNe observations * (e.g. Groenewegen 1997, Nozawa 2007) */ static const float representative_grain_size = 1e-5; /* Sputtering timescale normalisation in 1/s, following Tsai & Matthews (1995) */ static const double sputtering_timescale_norm = 3.2e-18; /* Fraction of zero age mass in stars above the SNII threshold for a * Chabrier (2000) IMF */ static const float SNII_mass_fraction = 7.039463e-3; /* Normalisation of gas mass swept by SNII shocks in from Yamasawa et. al * (2011), 1000 solar masses */ static const double snii_destruction_coeff = 3.052e+36; /* =============================== * ======== T20 specific ========= * =============================== */ /* Solar abundance pattern, assuming Wiersma et al (2009a) */ static const float solar_abundance_H = 7.0649785e-01; static const float solar_abundance_He = 2.8055534e-01; static const float solar_abundance_C = 2.0665436e-03; static const float solar_abundance_N = 8.3562563e-04; static const float solar_abundance_O = 5.4926244e-03; static const float solar_abundance_Ne = 1.4144605e-03; static const float solar_abundance_Mg = 5.9070642e-04; static const float solar_abundance_Si = 6.8258739e-04; static const float solar_abundance_Fe = 1.1032152e-03; /* Atomic weights for traced element up to Fe */ static const float atomic_weight_H = 1.0079; static const float atomic_weight_He = 4.0026; static const float atomic_weight_C = 12.0107; static const float atomic_weight_N = 14.0067; static const float atomic_weight_O = 15.9994; static const float atomic_weight_Ne = 20.1797; static const float atomic_weight_Mg = 24.305; static const float atomic_weight_Si = 28.0855; static const float atomic_weight_Fe = 55.845; /* Define the fiducial diffuse (i.e. complement of fiducial depleted) * fractions of elements constituting dust. These are taken from the * table dust assumptions for MW-like ISM conditions, and are scaled * by some factor to put a limit on depletion */ static const float fiducial_diffuse_C = 0.34385; static const float fiducial_diffuse_O = 0.31766; static const float fiducial_diffuse_Mg = 0.94338; static const float fiducial_diffuse_Si = 0.94492; static const float fiducial_diffuse_Fe = 0.99363; /* values determining the number of elements in ech effective grain * chemistry */ static const int atomicity_graphite = 1; static const int atomicity_silicate = 4; static const int atomicity_mgsilicate = 3; static const int atomicity_fesilicate = 3; /* Accretion timescale normalisation in seconds. Taken from the * default values of Hirashita & Voschinnikov (2013) */ static const float graphite_accretion_timescale_norm = 3.132e15; static const float silicate_accretion_timescale_norm = 5.677e15; /* Unitless condensation efficiencies for grains out of SNII outflow, * taken from Zhukovska et al (2008) */ static const float graphite_condensation_efficiency = 0.15; static const float silicate_condensation_efficiency = 3.5e-4; /* Shattering timescale normalisation in seconds. Taken from the * default values of Aoyama et al (2017, App. A.) */ static const double shattering_timescale_norm = 1.706e15; /* Coagulation timescale normalisation derived from Yan et al. * (2004), in s. */ static const double coagulation_timescale_norm = 1.709e13; // 4.273e14 // static const double coagulation_velocity_norm = 2e4; /* radius scaling factor relative to the fiducial 0.1 micron value */ static const float radius_scaling_large = 1.; static const float radius_scaling_small = 0.1; /* ------------ Parameter Defaults ------------ */ /* Default clumping factor */ static const float default_clumping_factor = 10.; /* Default number fraction of iron (as opposed to magnesium) grains */ static const float default_fe_grain_fraction = 0.5; /* Default fractions of injected grain sizes*/ static const float default_injection_fraction_large = 0.9; static const float default_injection_fraction_small = 0.1; /* Default silicate composition (olivine-like) */ static const float default_subscript_silicate_O = 6.; static const float default_subscript_silicate_Mg = 1.; static const float default_subscript_silicate_Si = 2.; static const float default_subscript_silicate_Fe = 1.; /* Factor to scale fiducial diffuse fractions by to limit depletion */ static const float default_diffuse_fraction_scaling = 0.423345; #endif /* SWIFT_DUST_CONSTANTS_H */