#ifndef SWIFT_DUST_M16_PROPERTIES_H
#define SWIFT_DUST_M16_PROPERTIES_H

/* Config parameters. */
#include <config.h>

/* Standard includes */
#include <hdf5.h>

/* Local includes. */
#include "chemistry_struct.h"
#include "cooling_properties.h"
#include "dust_struct.h"
#include "feedback_properties.h"
#include "physical_constants.h"
#include "units.h"

/**
 * @brief Stores AGB and SNII dust yields
 */

struct dust_yield_table {

  /* Array to read dust yield tables into */
  /* double *yield; */

  /* Array to store IMF-resampled dust yield tables */
  double* yield_IMF_resampled;
};

/**
 * @brief Properties of the dust evolution model.
 */
struct dustevo_props {

  /* ------------ Main operation modes ------------- */

  /*! Are we doing grain destruction by sputtering? */
  int with_sputtering;

  /*! Are we doing grain destruction by SNII? */
  int with_SNII_destruction;

  /*! Are we doing grain growth by accretion? */
  int with_accretion;

  /*! Are we using the subgrid T and rho? */
  int with_subgrid_props;

  /*! Are we pairing the dust fractions to cooling? */
  int pair_to_cooling;

  /* ------------ Global parameters ------------- */

  /*! Clumping factor assumed for accretion at a given density (default 10.)*/
  float clumping_factor;

  /*! Boost (> 1.) or reduction (< 1.) factor applied to dust diffusion rates
   * (default 1.) */
  float diffusion_rate_boost;

  /*! Fraction of Fe silicate grains (fayalite) as opposed to Mg (forsterite)
   * (default 0.5)*/
  float nu;

  /* ----------- Correcting cooling tables ---------- */

  /* array of element fractions assumed to be in the dust-phase */
  float* logfD;

  /* ------------ Dust yield tables ----------------- */

  /* Yield tables for AGB and SNII  */
  struct dust_yield_table dyield_AGB;
  struct dust_yield_table dyield_SNII;

  /* ------------- Dust Mapping -------------------- */

  /* metallicity of the Sun */
  float solar_metallicity;

  /* number of SNII per unit stellar mass */
  float specific_numSNII;

  /* initial abundance of dust species */
  float initial_grain_mass_fraction[dust_grain_species_count];

  /* mass fraction of each grain type constituted by given element */
  float* grain_element_mfrac[dust_grain_species_count];

  /* indices of chemistry array for element contributing to each grain */
  int* grain_element_indices[dust_grain_species_count];

  /* set element count contributing to each grain */
  int grain_element_count[dust_grain_species_count];

  /* Wiersma solar abundance patterns, for consistency with chemical yields */
  double abundance_pattern[chemistry_element_count];

  /* Element atomic weights */
  float atomic_weight[chemistry_element_count];

  /* Element condensation fractions */
  float condensation_frac[dust_grain_species_count];
};

void dustevo_props_init_backend(struct dustevo_props* dp,
                                struct swift_params* params,
                                struct feedback_props* fp,
                                struct cooling_function_data* cooling,
                                const struct phys_const* phys_const,
                                const struct unit_system* us);

/**
 * @brief Rescales COLIBRE cooling / heating rates using depletions.
 *
 * This is because values in abundances arrays become entirely
 * gas-phase when running with dust (ie. no implicit dust as in
 * COLIBRE and COLIBRE-CHIMES cooling)
 *
 * @param dustevo_properties
 */
static INLINE void generate_dust_yield_tables(struct dustevo_props* dp,
                                              struct feedback_props* fp) {

  /**
   * First read in tables for Dell'Aglia+19 AGB dust yields. These are
   * in the same format as the Wiersma+09 chemical yields.
   * yields are stored in dp->dyield_AGB
   *
   * Then, remove the yielded dust mass from the corresponding chemical
   * elements, according to each grain composition
   *
   * Finally, SNII dust yields are computed directly from chemical yields
   * following Zhukovska, Gail & Trieloff 2008. Again, corresponding mass
   * is removed from chemical yields, accounting for modification factors
   *
   * Currently, no SNIa dust creation is assumed
   **/
  ;
}

/* static INLINE void scale_out_table_depletion(struct cooling_function_data*
 * cooling){ */
/*   /\** */
/*    * Here, iterate through the 5 axes of the cooling table, scaling out */
/*    * depletion factors, as:  */
/*    * */
/*    * Theating[idx] -= log10(1-pow(10, table->log10fD[idx])) */
/*    * */
/*    * and */
/*    * */
/*    * Tcooling[idx] -= log10(1-pow(10, table->log10fD[idx])) */
/*    * */
/*    * Where table->log10fD are depletion factors that need to be read in  */
/*    * from the COLIBRE tables. */
/*    * */
/*    * Better to house this function in the cooling/COLIBRE and cooling/CHIMES
 */
/*    * code? Need to modify cooling code anyway to read table depletions. */
/*    **\/ */
/*   message("Scale out COLIBRE depletion from cooling/heating rates..."); */
/* } */

#endif /* SWIFT_DUST_M16_PROPERTIES_H */