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Commit 36c89901 authored by Matthieu Schaller's avatar Matthieu Schaller
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Can run the isolated galaxy with SNII feedback on.

parent 36656159
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examples/IsolatedGalaxy/IsolatedGalaxy_feedback/isolated_galaxy.yml
View file @ 36c89901
# Define the system of units to use internally.
InternalUnitSystem:
UnitMass_in_cgs: 1.9891E43 # 10^10 solar masses
UnitMass_in_cgs: 1.98848e43 # 10^10 M_sun in grams
UnitLength_in_cgs: 3.08567758E21 # 1 kpc
UnitVelocity_in_cgs: 1E5 # km/s
UnitCurrent_in_cgs: 1 # Amperes
......@@ -45,6 +45,7 @@ SPH:
CFL_condition: 0.1 # Courant-Friedrich-Levy condition for time integration.
h_min_ratio: 0.1 # Minimal smoothing in units of softening.
h_max: 10.
minimal_temperature: 100.
# Standard EAGLE cooling options
EAGLECooling:
......@@ -110,10 +111,7 @@ EAGLEEntropyFloor:
Cool_gamma_effective: 1. # Slope the of the EAGLE Cool limiter entropy floor
EAGLEFeedback:
filename: ./yieldtables/
imf_model: Chabrier
continuous_heating_switch: 0
SNIa_timescale_Gyr: 2.0
SNIa_efficiency: 2.e-3
SNII_wind_delay_Gyr: 0.03
SNe_heating_temperature_K: 3.16228e7
filename: ./yieldtables/
SNII_wind_delay_Gyr: 0.0001
SNII_delta_T_K: 3.16228e7
SNII_Energy_erg: 1.0e51
src/cell.c
View file @ 36c89901
......@@ -53,6 +53,7 @@
#include "drift.h"
#include "engine.h"
#include "error.h"
#include "feedback.h"
#include "gravity.h"
#include "hydro.h"
#include "hydro_properties.h"
......@@ -4366,6 +4367,7 @@ void cell_drift_spart(struct cell *c, const struct engine *e, int force) {
/* Get ready for a density calculation */
if (spart_is_active(sp, e)) {
stars_init_spart(sp);
feedback_init_spart(sp);
}
}
......
src/feedback/EAGLE/feedback.c
View file @ 36c89901
......@@ -27,25 +27,113 @@
#include "yield_tables.h"
/**
* @brief Compute number of SN that should go off given the age of the spart
* @brief Return the change in temperature (in internal units) to apply to a
* gas particle affected by SNe feedback.
*
* @param sp spart we're evolving
* @param stars_properties stars_props data structure
* @param age age of star at the beginning of the step
* @param dt length of step
* @param sp The #spart.
* @param props The properties of the feedback model.
*/
float compute_SNe(const struct spart* sp,
const struct feedback_props* feedback_props, const float age,
const float dt) {
double eagle_feedback_temperature_change(const struct spart* sp,
const struct feedback_props* props) {
/* In the EAGLE REF model, the change of temperature is constant */
return props->SNe_deltaT_desired;
}
/**
* @brief Computes the number of super-novae exploding for a given
* star particle.
*
* @param sp The #spart.
* @param props The properties of the stellar model.
*/
double eagle_feedback_number_of_SNe(const struct spart* sp,
const struct feedback_props* props) {
message("init_mass=%e conv=%e N/Msun=%e", sp->mass_init,
props->mass_to_solar_mass, props->num_SNII_per_msun);
/* Note: For a Chabrier 2003 IMF and SNII going off between 6 and 100
* M_sun, the first term is 0.017362 M_sun^-1 */
return props->num_SNII_per_msun * sp->mass_init * props->mass_to_solar_mass;
}
/**
* @brief Computes the fraction of the available super-novae energy to
* inject for a given event.
*
* Note that the fraction can be > 1.
*
* @param sp The #spart.
* @param props The properties of the feedback model.
*/
double eagle_feedback_energy_fraction(const struct spart* sp,
const struct feedback_props* props) {
return 1.;
}
/**
* @brief Compute the properties of the SNe feedback energy injection.
*
* Only does something if the particle reached the SNe age during this time
* step.
*
* @param sp The star particle.
* @param feedback_props The properties of the feedback model.
* @param star_age Age of star at the beginning of the step in internal units.
* @param dt Length of time-step in internal units.
*/
inline static void compute_SNe_feedback(
struct spart* sp, const double star_age, const double dt,
const struct feedback_props* feedback_props) {
/* Time after birth considered for SNII feedback (internal units) */
const float SNII_wind_delay = feedback_props->SNII_wind_delay;
if (age <= SNII_wind_delay && (age + dt) > SNII_wind_delay) {
/* Are we doing feedback this step? */
if (star_age <= SNII_wind_delay && (star_age + dt) > SNII_wind_delay) {
return feedback_props->num_SNII_per_msun * sp->mass_init /
feedback_props->const_solar_mass;
} else {
return 0.f;
/* Properties of the model (all in internal units) */
const double delta_T =
eagle_feedback_temperature_change(sp, feedback_props);
const double N_SNe = eagle_feedback_number_of_SNe(sp, feedback_props);
const double E_SNe = feedback_props->E_SNII;
const double f_E = eagle_feedback_energy_fraction(sp, feedback_props);
/* Conversion factor from T to internal energy */
const double conv_factor = feedback_props->temp_to_u_factor;
/* Calculate the default heating probability */
double prob = f_E * E_SNe * N_SNe /
(conv_factor * delta_T * sp->feedback_data.ngb_mass);
/* Calculate the change in internal energy of the gas particles that get
* heated */
double delta_u;
if (prob <= 1.) {
/* Normal case */
delta_u = delta_T * conv_factor;
} else {
/* Special case: we need to adjust the energy irrespective of the
desired deltaT to ensure we inject all the available energy. */
prob = 1.;
delta_u = f_E * E_SNe * N_SNe / sp->feedback_data.ngb_mass;
}
message(
"ID=%lld E_SNe=%e N_SNe=%e deltaT= %e f_E=%e prob=%f ngb_mass=%f "
"fac=%e delta_u=%e",
sp->id, E_SNe, N_SNe, delta_T, f_E, prob, sp->feedback_data.ngb_mass,
conv_factor, delta_u);
/* Store all of this in the star for delivery onto the gas */
sp->feedback_data.to_distribute.SNII_heating_probability = prob;
sp->feedback_data.to_distribute.SNII_delta_u = delta_u;
}
}
......@@ -182,53 +270,59 @@ inline static void evolve_SNIa(float log10_min_mass, float log10_max_mass,
struct spart* restrict sp, float star_age_Gyr,
float dt_Gyr) {
/* Check if we're outside the mass range for SNIa */
if (log10_min_mass >= feedback_props->log10_SNIa_max_mass_msun) return;
/* If the max mass is outside the mass range update it to be the maximum and
* use updated values for the star's age and timestep in this function */
if (log10_max_mass > feedback_props->log10_SNIa_max_mass_msun) {
log10_max_mass = feedback_props->log10_SNIa_max_mass_msun;
float lifetime_Gyr = lifetime_in_Gyr(
exp(M_LN10 * feedback_props->log10_SNIa_max_mass_msun),
sp->chemistry_data.metal_mass_fraction_total, feedback_props);
dt_Gyr = star_age_Gyr + dt_Gyr - lifetime_Gyr;
star_age_Gyr = lifetime_Gyr;
}
/* /\* Check if we're outside the mass range for SNIa *\/ */
/* if (log10_min_mass >= feedback_props->log10_SNIa_max_mass_msun) return; */
/* compute the number of SNIa */
/* Efolding (Forster 2006) */
float num_SNIa_per_msun =
feedback_props->SNIa_efficiency *
(exp(-star_age_Gyr / feedback_props->SNIa_timescale_Gyr) -
exp(-(star_age_Gyr + dt_Gyr) / feedback_props->SNIa_timescale_Gyr)) *
sp->mass_init;
sp->feedback_data.to_distribute.num_SNIa =
num_SNIa_per_msun / feedback_props->const_solar_mass;
/* compute mass fractions of each metal */
for (int i = 0; i < chemistry_element_count; i++) {
sp->feedback_data.to_distribute.metal_mass[i] +=
num_SNIa_per_msun * feedback_props->yield_SNIa_IMF_resampled[i];
}
/* /\* If the max mass is outside the mass range update it to be the maximum
* and */
/* * use updated values for the star's age and timestep in this function *\/
*/
/* if (log10_max_mass > feedback_props->log10_SNIa_max_mass_msun) { */
/* log10_max_mass = feedback_props->log10_SNIa_max_mass_msun; */
/* float lifetime_Gyr = lifetime_in_Gyr( */
/* exp(M_LN10 * feedback_props->log10_SNIa_max_mass_msun), */
/* sp->chemistry_data.metal_mass_fraction_total, feedback_props); */
/* dt_Gyr = star_age_Gyr + dt_Gyr - lifetime_Gyr; */
/* star_age_Gyr = lifetime_Gyr; */
/* } */
/* Update the metallicity of the material released */
sp->feedback_data.to_distribute.metal_mass_from_SNIa +=
num_SNIa_per_msun * feedback_props->yield_SNIa_total_metals_IMF_resampled;
/* /\* compute the number of SNIa *\/ */
/* /\* Efolding (Forster 2006) *\/ */
/* float num_SNIa_per_msun = */
/* feedback_props->SNIa_efficiency * */
/* (exp(-star_age_Gyr / feedback_props->SNIa_timescale_Gyr) - */
/* exp(-(star_age_Gyr + dt_Gyr) / feedback_props->SNIa_timescale_Gyr)) *
*/
/* sp->mass_init; */
/* Update the metal mass produced */
sp->feedback_data.to_distribute.total_metal_mass +=
num_SNIa_per_msun * feedback_props->yield_SNIa_total_metals_IMF_resampled;
/* sp->feedback_data.to_distribute.num_SNIa = */
/* num_SNIa_per_msun / feedback_props->const_solar_mass; */
/* Compute the mass produced by SNIa */
sp->feedback_data.to_distribute.mass_from_SNIa +=
num_SNIa_per_msun * feedback_props->yield_SNIa_total_metals_IMF_resampled;
/* /\* compute mass fractions of each metal *\/ */
/* for (int i = 0; i < chemistry_element_count; i++) { */
/* sp->feedback_data.to_distribute.metal_mass[i] += */
/* num_SNIa_per_msun * feedback_props->yield_SNIa_IMF_resampled[i]; */
/* } */
/* Compute the iron mass produced */
sp->feedback_data.to_distribute.Fe_mass_from_SNIa +=
num_SNIa_per_msun *
feedback_props->yield_SNIa_IMF_resampled[chemistry_element_Fe];
/* /\* Update the metallicity of the material released *\/ */
/* sp->feedback_data.to_distribute.metal_mass_from_SNIa += */
/* num_SNIa_per_msun *
* feedback_props->yield_SNIa_total_metals_IMF_resampled; */
/* /\* Update the metal mass produced *\/ */
/* sp->feedback_data.to_distribute.total_metal_mass += */
/* num_SNIa_per_msun *
* feedback_props->yield_SNIa_total_metals_IMF_resampled; */
/* /\* Compute the mass produced by SNIa *\/ */
/* sp->feedback_data.to_distribute.mass_from_SNIa += */
/* num_SNIa_per_msun *
* feedback_props->yield_SNIa_total_metals_IMF_resampled; */
/* /\* Compute the iron mass produced *\/ */
/* sp->feedback_data.to_distribute.Fe_mass_from_SNIa += */
/* num_SNIa_per_msun * */
/* feedback_props->yield_SNIa_IMF_resampled[chemistry_element_Fe]; */
}
/**
......@@ -560,7 +654,7 @@ void compute_stellar_evolution(const struct feedback_props* feedback_props,
const float dt) {
/* Allocate temporary array for calculating imf weights */
float stellar_yields[eagle_feedback_N_imf_bins];
// float stellar_yields[eagle_feedback_N_imf_bins];
/* Convert dt and stellar age from internal units to Gyr. */
const double Gyr_in_cgs = 1e9 * 365. * 24. * 3600.;
......@@ -572,7 +666,10 @@ void compute_stellar_evolution(const struct feedback_props* feedback_props,
/* Get the metallicity */
const float Z = sp->chemistry_data.metal_mass_fraction_total;
/* calculate mass of stars that has died from the star's birth up to the
/* Compute properties of the stochastic SNe feedback model. */
compute_SNe_feedback(sp, age, dt, feedback_props);
/* Calculate mass of stars that has died from the star's birth up to the
* beginning and end of timestep */
const float max_dying_mass_Msun =
dying_mass_msun(star_age_Gyr, Z, feedback_props);
......@@ -592,42 +689,45 @@ void compute_stellar_evolution(const struct feedback_props* feedback_props,
if (min_dying_mass_Msun == max_dying_mass_Msun) return;
/* Life is better in log */
const float log10_max_dying_mass_Msun = log10f(max_dying_mass_Msun);
const float log10_min_dying_mass_Msun = log10f(min_dying_mass_Msun);
/* Compute elements, energy and momentum to distribute from the
* three channels SNIa, SNII, AGB */
evolve_SNIa(log10_min_dying_mass_Msun, log10_max_dying_mass_Msun,
feedback_props, sp, star_age_Gyr, dt_Gyr);
evolve_SNII(log10_min_dying_mass_Msun, log10_max_dying_mass_Msun,
stellar_yields, feedback_props, sp);
evolve_AGB(log10_min_dying_mass_Msun, log10_max_dying_mass_Msun,
stellar_yields, feedback_props, sp);
/* Compute the total mass to distribute (H + He metals) */
sp->feedback_data.to_distribute.mass =
sp->feedback_data.to_distribute.total_metal_mass +
sp->feedback_data.to_distribute.metal_mass[chemistry_element_H] +
sp->feedback_data.to_distribute.metal_mass[chemistry_element_He];
/* Compute the number of type II SNe that went off */
sp->feedback_data.to_distribute.num_SNe =
compute_SNe(sp, feedback_props, age, dt);
/* Compute energy change due to thermal and kinetic energy of ejecta */
sp->feedback_data.to_distribute.d_energy =
sp->feedback_data.to_distribute.mass *
(feedback_props->ejecta_specific_thermal_energy +
0.5 * (sp->v[0] * sp->v[0] + sp->v[1] * sp->v[1] + sp->v[2] * sp->v[2]) *
cosmo->a2_inv);
/* Compute probability of heating neighbouring particles */
if (dt > 0 && sp->feedback_data.ngb_mass > 0)
sp->feedback_data.to_distribute.heating_probability =
feedback_props->total_energy_SNe *
sp->feedback_data.to_distribute.num_SNe /
(feedback_props->temp_to_u_factor * feedback_props->SNe_deltaT_desired *
sp->feedback_data.ngb_mass);
/* const float log10_max_dying_mass_Msun = log10f(max_dying_mass_Msun); */
/* const float log10_min_dying_mass_Msun = log10f(min_dying_mass_Msun); */
/* /\* Compute elements, energy and momentum to distribute from the */
/* * three channels SNIa, SNII, AGB *\/ */
/* evolve_SNIa(log10_min_dying_mass_Msun, log10_max_dying_mass_Msun, */
/* feedback_props, sp, star_age_Gyr, dt_Gyr); */
/* evolve_SNII(log10_min_dying_mass_Msun, log10_max_dying_mass_Msun, */
/* stellar_yields, feedback_props, sp); */
/* evolve_AGB(log10_min_dying_mass_Msun, log10_max_dying_mass_Msun, */
/* stellar_yields, feedback_props, sp); */
/* /\* Compute the total mass to distribute (H + He metals) *\/ */
/* sp->feedback_data.to_distribute.mass = */
/* sp->feedback_data.to_distribute.total_metal_mass + */
/* sp->feedback_data.to_distribute.metal_mass[chemistry_element_H] + */
/* sp->feedback_data.to_distribute.metal_mass[chemistry_element_He]; */
/* /\* Compute energy change due to thermal and kinetic energy of ejecta *\/
*/
/* sp->feedback_data.to_distribute.d_energy = */
/* sp->feedback_data.to_distribute.mass * */
/* (feedback_props->ejecta_specific_thermal_energy + */
/* 0.5 * (sp->v[0] * sp->v[0] + sp->v[1] * sp->v[1] + sp->v[2] *
* sp->v[2]) * */
/* cosmo->a2_inv); */
/* /\* Compute the number of type II SNe that went off *\/ */
/* sp->feedback_data.to_distribute.num_SNe = */
/* compute_SNe(sp, feedback_props, age, dt); */
/* /\* Compute probability of heating neighbouring particles *\/ */
/* if (dt > 0 && sp->feedback_data.ngb_mass > 0) */
/* sp->feedback_data.to_distribute.heating_probability = */
/* feedback_props->total_energy_SNe * */
/* sp->feedback_data.to_distribute.num_SNe / */
/* (feedback_props->temp_to_u_factor *
* feedback_props->SNe_deltaT_desired * */
/* sp->feedback_data.ngb_mass); */
}
/**
......@@ -648,17 +748,13 @@ void feedback_props_init(struct feedback_props* fp,
const struct hydro_props* hydro_props,
const struct cosmology* cosmo) {
/* Read SNIa timscale */
fp->SNIa_timescale_Gyr =
parser_get_param_float(params, "EAGLEFeedback:SNIa_timescale_Gyr");
/* /\* Read SNIa timscale *\/ */
/* fp->SNIa_timescale_Gyr = */
/* parser_get_param_float(params, "EAGLEFeedback:SNIa_timescale_Gyr"); */
/* Read the efficiency of producing SNIa */
fp->SNIa_efficiency =
parser_get_param_float(params, "EAGLEFeedback:SNIa_efficiency");
/* Are we doing continuous heating? */
fp->continuous_heating =
parser_get_param_int(params, "EAGLEFeedback:continuous_heating_switch");
/* /\* Read the efficiency of producing SNIa *\/ */
/* fp->SNIa_efficiency = */
/* parser_get_param_float(params, "EAGLEFeedback:SNIa_efficiency"); */
/* Set the delay time before SNII occur */
const float Gyr_in_cgs = 1e9 * 365 * 24 * 3600;
......@@ -666,36 +762,43 @@ void feedback_props_init(struct feedback_props* fp,
parser_get_param_float(params, "EAGLEFeedback:SNII_wind_delay_Gyr") *
Gyr_in_cgs / units_cgs_conversion_factor(us, UNIT_CONV_TIME);
message("Wind delay: %e", fp->SNII_wind_delay);
/* Read the temperature change to use in stochastic heating */
fp->SNe_deltaT_desired =
parser_get_param_float(params, "EAGLEFeedback:SNe_heating_temperature_K");
parser_get_param_float(params, "EAGLEFeedback:SNII_delta_T_K");
fp->SNe_deltaT_desired /=
units_cgs_conversion_factor(us, UNIT_CONV_TEMPERATURE);
/* Energy released by supernova type II */
fp->E_SNII_cgs =
parser_get_param_double(params, "EAGLEFeedback:SNII_Energy_erg");
fp->E_SNII =
fp->E_SNII_cgs / units_cgs_conversion_factor(us, UNIT_CONV_ENERGY);
/* Gather common conversion factors */
/* Calculate internal mass to solar mass conversion factor */
const double Msun_cgs = phys_const->const_solar_mass *
units_cgs_conversion_factor(us, UNIT_CONV_MASS);
const double unit_mass_cgs = units_cgs_conversion_factor(us, UNIT_CONV_MASS);
fp->mass_to_solar_mass = unit_mass_cgs / Msun_cgs;
/* Calculate temperature to internal energy conversion factor (all internal
* units) */
const double k_B = phys_const->const_boltzmann_k;
const double m_p = phys_const->const_proton_mass;
const double mu = hydro_props->mu_ionised;
fp->temp_to_u_factor = k_B / (mu * hydro_gamma_minus_one * m_p);
// MATTHIEU up to here
/* Set ejecta thermal energy */
const float ejecta_velocity =
1.0e6 / units_cgs_conversion_factor(
us, UNIT_CONV_SPEED); // EAGLE parameter is 10 km/s
fp->ejecta_specific_thermal_energy = 0.5 * ejecta_velocity * ejecta_velocity;
/* Energy released by supernova */
fp->total_energy_SNe =
1.0e51 / units_cgs_conversion_factor(us, UNIT_CONV_ENERGY);
/* Calculate temperature to internal energy conversion factor */
fp->temp_to_u_factor =
phys_const->const_boltzmann_k /
(hydro_props->mu_ionised *
(hydro_gamma_minus_one)*phys_const->const_proton_mass);
/* Read birth time to set all stars in ICs to (defaults to -1 to indicate star
* present in ICs) */
fp->spart_first_init_birth_time = parser_get_opt_param_float(
params, "EAGLEFeedback:birth_time_override", -1);
/* Copy over solar mass */
fp->const_solar_mass = phys_const->const_solar_mass;
/* Set number of elements found in yield tables */
fp->lifetimes.n_mass = 30;
fp->lifetimes.n_z = 6;
......@@ -745,12 +848,13 @@ void feedback_props_init(struct feedback_props* fp,
* mass bins used in IMF */
compute_ejecta(fp);
/* Calculate number of type II SN per solar mass
* Note: since we are integrating the IMF without weighting it by the yields
* pass NULL pointer for stellar_yields array */
fp->num_SNII_per_msun = integrate_imf(fp->log10_SNII_min_mass_msun,
fp->log10_SNII_max_mass_msun, 0,
/*(stellar_yields=)*/ NULL, fp);
/* Calculate number of type II SN per unit solar mass based on our choice
* of IMF and integration limits for type II SNe.
* Note: No weighting by yields here. */
fp->num_SNII_per_msun =
integrate_imf(fp->log10_SNII_min_mass_msun, fp->log10_SNII_max_mass_msun,
eagle_imf_integration_no_weight,
/*(stellar_yields=)*/ NULL, fp);
message("initialized stellar feedback");
}
src/feedback/EAGLE/feedback.h
View file @ 36c89901
......@@ -20,6 +20,7 @@
#define SWIFT_FEEDBACK_EAGLE_H
#include "cosmology.h"
#include "error.h"
#include "feedback_properties.h"
#include "hydro_properties.h"
#include "part.h"
......@@ -94,8 +95,11 @@ __attribute__((always_inline)) INLINE static void feedback_prepare_spart(
/* Zero the energy to inject */
sp->feedback_data.to_distribute.d_energy = 0.f;
/* Zero the feedback probability */
sp->feedback_data.to_distribute.heating_probability = 0.f;
/* Zero the SNII feedback probability */
sp->feedback_data.to_distribute.SNII_heating_probability = 0.f;
/* Zero the SNII feedback energy */
sp->feedback_data.to_distribute.SNII_delta_u = 0.f;
}
/**
......
src/feedback/EAGLE/feedback_iact.h
View file @ 36c89901
......@@ -56,18 +56,14 @@ runner_iact_nonsym_feedback_density(float r2, const float *dx, float hi,
kernel_eval(ui, &wi);
/* Add mass of pj to neighbour mass of si */
si->feedback_data.ngb_mass += hydro_get_mass(pj);
si->feedback_data.ngb_mass += mj;
/* Add contribution of pj to normalisation of density weighted fraction
* which determines how much mass to distribute to neighbouring
* gas particles */
const float rho = hydro_get_comoving_density(pj);
if (rho != 0)
si->feedback_data.density_weighted_frac_normalisation_inv += wi / rho;
/* Compute contribution to the density */
si->rho_gas += mj * wi;
// const float rho = hydro_get_comoving_density(pj);
// si->feedback_data.density_weighted_frac_normalisation_inv += wi / rho;
}
/**
......@@ -104,153 +100,167 @@ runner_iact_nonsym_feedback_apply(
float wi;
kernel_eval(ui, &wi);
/* Compute weighting for distributing feedback quantities */
float density_weighted_frac;
float rho = hydro_get_comoving_density(pj);
if (rho * si->feedback_data.density_weighted_frac_normalisation_inv != 0) {
density_weighted_frac =
wi / (rho * si->feedback_data.density_weighted_frac_normalisation_inv);
} else {
density_weighted_frac = 0.f;
}
/* /\* Compute weighting for distributing feedback quantities *\/ */
/* float density_weighted_frac; */
/* float rho = hydro_get_comoving_density(pj); */
/* if (rho * si->feedback_data.density_weighted_frac_normalisation_inv != 0) {
*/
/* density_weighted_frac = */
/* wi / (rho *
* si->feedback_data.density_weighted_frac_normalisation_inv); */
/* } else { */
/* density_weighted_frac = 0.f; */
/* } */
/* Update particle mass */
const float current_mass = hydro_get_mass(pj);
const float new_mass = current_mass + si->feedback_data.to_distribute.mass *
density_weighted_frac;
hydro_set_mass(pj, new_mass);
/* Update total metallicity */
const float current_metal_mass_total =
pj->chemistry_data.metal_mass_fraction_total * current_mass;
const float new_metal_mass_total =
current_metal_mass_total +
si->feedback_data.to_distribute.total_metal_mass * density_weighted_frac;
pj->chemistry_data.metal_mass_fraction_total =
new_metal_mass_total / new_mass;
/* Update mass fraction of each tracked element */
for (int elem = 0; elem < chemistry_element_count; elem++) {
const float current_metal_mass =
pj->chemistry_data.metal_mass_fraction[elem] * current_mass;
const float new_metal_mass =
current_metal_mass + si->feedback_data.to_distribute.metal_mass[elem] *
density_weighted_frac;
pj->chemistry_data.metal_mass_fraction[elem] = new_metal_mass / new_mass;
}
/* /\* Update particle mass *\/ */
/* const float current_mass = hydro_get_mass(pj); */
/* const float new_mass = current_mass + si->feedback_data.to_distribute.mass
* * */
/* density_weighted_frac; */
/* Update iron mass fraction from SNIa */
const float current_iron_from_SNIa_mass =
pj->chemistry_data.iron_mass_fraction_from_SNIa * current_mass;
const float new_iron_from_SNIa_mass =
current_iron_from_SNIa_mass +
si->feedback_data.to_distribute.Fe_mass_from_SNIa * density_weighted_frac;
pj->chemistry_data.iron_mass_fraction_from_SNIa =
new_iron_from_SNIa_mass / new_mass;
/* Update mass fraction from SNIa */
const float current_mass_from_SNIa =
pj->chemistry_data.mass_from_SNIa * current_mass;
const float new_mass_from_SNIa =
current_mass_from_SNIa +
si->feedback_data.to_distribute.mass_from_SNIa * density_weighted_frac;
pj->chemistry_data.mass_from_SNIa = new_mass_from_SNIa / new_mass;
/* Update metal mass fraction from SNIa */
const float current_metal_mass_fraction_from_SNIa =
pj->chemistry_data.metal_mass_fraction_from_SNIa * current_mass;
const float new_metal_mass_fraction_from_SNIa =
current_metal_mass_fraction_from_SNIa +
si->feedback_data.to_distribute.metal_mass_from_SNIa *
density_weighted_frac;
pj->chemistry_data.metal_mass_fraction_from_SNIa =
new_metal_mass_fraction_from_SNIa / new_mass;
/* Update mass fraction from SNII */
const float current_mass_from_SNII =
pj->chemistry_data.mass_from_SNII * current_mass;
const float new_mass_from_SNII =
current_mass_from_SNII +
si->feedback_data.to_distribute.mass_from_SNII * density_weighted_frac;
pj->chemistry_data.mass_from_SNII = new_mass_from_SNII / new_mass;
/* Update metal mass fraction from SNII */
const float current_metal_mass_fraction_from_SNII =