double collisional_starburst_recipe(double mass_ratio, int merger_centralgal, int centralgal,
double time, double deltaT, int nstep) //ROB: New variable 'nstep' added, for use in update_yields()
{
/** @brief If StarBurstRecipe = 1 (since Croton2006), the Somerville 2001
* model of bursts is used. The burst can happen for both major
* and minor mergers, with a fraction of the added cold gas from
* the satellite and central being consumed. SN Feedback from
* starformation is computed and the sizes of bulge and disk
* followed (not done for the other burst mode).*/
double mstars, reheated_mass, ejected_mass, fac, metallicitySF;
double CentralVvir, eburst, MergeCentralVvir, Ggas, EjectVmax, EjectVvir;
double SN_Energy, Reheat_Energy;
/* This is the major and minor merger starburst recipe of Somerville 2001.
* The coefficients in eburst are taken from TJ Cox's PhD thesis and should
* be more accurate then previous. */
Ggas=Gal[merger_centralgal].ColdGas;
/* the bursting fraction given the mass ratio */
/* m_dot = 0.56*(m_sat/m_central)^0.7*m_gas */
eburst = SfrBurstEfficiency * pow(mass_ratio, SfrBurstSlope);
//eburst = 0.56 * pow(mass_ratio, 0.7);
mstars = eburst * Gal[merger_centralgal].ColdGas;
if(mstars < 0.0)
mstars = 0.0;
/* this bursting results in SN feedback on the cold/hot gas
* TODO this is the same code used in star_formation_and_feedback.c
* and should be merged if possible. */
if(FeedbackRecipe == 0 || FeedbackRecipe == 1) {
if (Gal[merger_centralgal].Type == 0)
reheated_mass = FeedbackReheatingEpsilon *
mstars*(.5+1./pow(Gal[merger_centralgal].Vmax/ReheatPreVelocity,ReheatSlope));
else
reheated_mass = FeedbackReheatingEpsilon *
mstars*(.5+1./pow(Gal[merger_centralgal].InfallVmax/ReheatPreVelocity,ReheatSlope));
}
//Make sure that the energy used does not exceed the SN energy (central subhalo Vvir used)
if(FeedbackRecipe == 0 || FeedbackRecipe == 1) {
if (reheated_mass * Gal[merger_centralgal].Vvir * Gal[merger_centralgal].Vvir > mstars * EtaSNcode * EnergySNcode)
reheated_mass = mstars * EtaSNcode * EnergySNcode / Gal[merger_centralgal].Vvir / Gal[merger_centralgal].Vvir;
}
/* cant use more cold gas than is available! so balance SF and feedback */
if((mstars + reheated_mass) > Gal[merger_centralgal].ColdGas) {
fac = Gal[merger_centralgal].ColdGas / (mstars + reheated_mass);
mstars *= fac;
reheated_mass *= fac;
}
if (merger_centralgal == centralgal)
{
EjectVmax=Gal[centralgal].Vmax;
EjectVvir=Gal[centralgal].Vvir;// main halo Vvir
}
else
{
EjectVmax=Gal[merger_centralgal].InfallVmax;
EjectVvir=Gal[merger_centralgal].Vvir; //central subhalo Vvir
}
/* determine ejection*/
if(FeedbackRecipe == 0) {
ejected_mass = (FeedbackEjectionEfficiency* (EtaSNcode * EnergySNcode) *mstars
* min(1./FeedbackEjectionEfficiency,.5+1/pow(EjectVmax/EjectPreVelocity,EjectSlope))
- reheated_mass*EjectVvir*EjectVvir) /(EjectVvir*EjectVvir);
}
else if(FeedbackRecipe == 1)
{
SN_Energy = .5 * mstars * (EtaSNcode * EnergySNcode);
Reheat_Energy = .5 * reheated_mass * EjectVvir * EjectVvir;
ejected_mass = (SN_Energy - Reheat_Energy)/(0.5 * FeedbackEjectionEfficiency*(EtaSNcode * EnergySNcode));
if(FeedbackEjectionEfficiency*(EtaSNcode * EnergySNcode)<EjectVvir*EjectVvir)
ejected_mass =0.0;
}
// Finished calculating mass exchanges, so just check that none are negative
if (reheated_mass < 0.0) reheated_mass = 0.0;
if (ejected_mass < 0.0) ejected_mass = 0.0;
/* update the star formation rate */
#ifdef SAVE_MEMORY
Gal[merger_centralgal].Sfr += mstars / deltaT;
#else
for(outputbin = 0; outputbin < NOUT; outputbin++) {
if(Halo[halonr].SnapNum == ListOutputSnaps[outputbin]) {
Gal[merger_centralgal].Sfr[outputbin] += mstars / deltaT;
break;
}
}
#endif
/* Store the value of the metallicity of the cold phase when SF occurs.
* Used to update luminosities below */
#ifdef METALS
//metallicitySF = Gal[merger_centralgal].MetalsColdGas.type2/Gal[merger_centralgal].ColdGas;
metallicitySF = metals_total(Gal[merger_centralgal].MetalsColdGas)/Gal[merger_centralgal].ColdGas;
#else
metallicitySF = Gal[merger_centralgal].MetalsColdGas/Gal[merger_centralgal].ColdGas;
#endif
mass_checks("collisional_starburst_recipe #1",merger_centralgal);
if (mstars > 0.)
update_from_star_formation(merger_centralgal, mstars, deltaT/STEPS, nstep);
mass_checks("collisional_starburst_recipe #2",merger_centralgal);
// Do not call if Gal[merger_centralgal].ColdGas < 1e-8?
if (reheated_mass + ejected_mass > 0.)
update_from_feedback(merger_centralgal, centralgal, reheated_mass, ejected_mass);
#ifndef POST_PROCESS_MAGS
/* update the luminosities due to the stars formed */
if (mstars > 0.0)
add_to_luminosities(merger_centralgal, mstars, time, metallicitySF);
#endif
if (Ggas > 0.)
return mstars/Ggas;
else
return 0.0;
}
/** @brief Main recipe, calculates the fraction of cold gas turned into stars due
* to star formation; the fraction of mass instantaneously recycled and
* returned to the cold gas; the fraction of gas reheated from cold to hot,
* ejected from hot to external and returned from ejected to hot due to
* SN feedback. */
void starformation(int p, int centralgal, double time, double dt, int nstep)
{
/*! Variables: reff-Rdisk, tdyn=Rdisk/Vmax, strdot=Mstar_dot, stars=strdot*dt*/
double tdyn, strdot=0., stars, cold_crit, metallicitySF;
if(Gal[p].Type == 0)
{
tdyn = Gal[p].GasDiskRadius / Gal[p].Vmax;
cold_crit = SfrColdCrit * Gal[p].Vmax/200. * Gal[p].GasDiskRadius*100.;
}
else
{
tdyn = Gal[p].GasDiskRadius / Gal[p].InfallVmax;
cold_crit = SfrColdCrit * Gal[p].InfallVmax/200. * Gal[p].GasDiskRadius*100.;
}
//standard star formation law (Croton2006, Delucia2007, Guo2010)
if(StarFormationModel == 0)
{
if(Gal[p].ColdGas > cold_crit)
strdot = SfrEfficiency * (Gal[p].ColdGas - cold_crit) / tdyn;
else
strdot = 0.0;
}
/*if(StarFormationModel == 1)
{
strdot = ALTERNATIVE STAR FORMATION LAW
}*/
/* Note that Units of dynamical time are Mpc/Km/s - no conversion on dt needed */
stars = strdot * dt;
if(stars < 0.0)
terminate("***error stars<0.0***\n");
//otherwise cold gas and stars share material in update_stars_due_to_reheat
#ifdef FEEDBACK_COUPLED_WITH_MASS_RETURN
if(stars > Gal[p].ColdGas)
stars = Gal[p].ColdGas;
#endif
mass_checks("recipe_starform #1",p);
mass_checks("recipe_starform #1.1",centralgal);
/* update for star formation
* updates Mcold, StellarMass, MetalsMcold and MetalsStellarMass
* in Guo2010 case updates the stellar spin -> hardwired, not an option */
/* Store the value of the metallicity of the cold phase when SF occurs */
if (Gal[p].ColdGas > 0.)
metallicitySF= metals_total(Gal[p].MetalsColdGas)/Gal[p].ColdGas;
else
metallicitySF=0.;
if (stars > 0.)
update_stars_due_to_reheat(p, centralgal, &stars);
mass_checks("recipe_starform #2",p);
mass_checks("recipe_starform #2.1",centralgal);
/* update the star formation rate */
/*Sfr=stars/(dt*steps)=strdot*dt/(dt*steps)=strdot/steps -> average over the STEPS*/
Gal[p].Sfr += stars / (dt * STEPS);
// update_from_star_formation can only be called
// after SD_feeedback recipe since stars need to be re_set once the reheated mass is known
// (star formation and feedback share the same fraction of cold gas)
if (stars > 0.)
update_from_star_formation(p, stars, false, nstep); // false indicates not a burst
update_massweightage(p, stars, time);
#ifndef FEEDBACK_COUPLED_WITH_MASS_RETURN
/* ifdef FEEDBACK_COUPLED_WITH_MASS_RETURN feedback is only called
* when stars die, inside DETAILED_METALS_AND_MASS_RETURN */
if (stars > 0.)
SN_feedback(p, centralgal, stars, "ColdGas");
#endif
#ifdef COMPUTE_SPECPHOT_PROPERTIES
#ifndef POST_PROCESS_MAGS
/* Update the luminosities due to the stars formed */
if (stars > 0.0)
add_to_luminosities(p, stars, time, dt, metallicitySF);
#endif //NDEF POST_PROCESS_MAGS
#endif //COMPUTE_SPECPHOT_PROPERTIES
if(Gal[p].DiskMass > 0.0)
check_disk_instability(p);
if (DiskRadiusModel== 0)
get_stellar_disk_radius(p);
}
void do_AGN_heating(double dt, int ngal)
{
double AGNrate, AGNheating, AGNaccreted, AGNcoeff, fraction, EDDrate, FreeFallRadius;
double dist, HotGas, HotRadius, Rvir, Vvir, Mvir;
double LeftOverEnergy, CoolingGas, AGNAccretedFromCentral;
int p, FoFCentralGal;
if(AGNRadioModeModel == 0)
{
for (p = 0; p < ngal; p++)
if(Gal[p].Type == 0)
FoFCentralGal=p;
}
for (p = 0; p < ngal; p++)
{
Gal[p].CoolingRate_beforeAGN += Gal[p].CoolingGas / (dt*STEPS);
AGNrate=0.;
LeftOverEnergy = 0.;
HotGas = Gal[p].HotGas;
HotRadius = Gal[p].HotRadius;
CoolingGas = Gal[p].CoolingGas;
Mvir = Gal[p].Mvir;
Rvir = Gal[p].Rvir;
Vvir = Gal[p].Vvir;
if(HotGas > 0.0)
{
if(AGNRadioModeModel == 0)
AGNrate = AgnEfficiency * (UnitTime_in_s*SOLAR_MASS)/(UNITMASS_IN_G*SEC_PER_YEAR)
* Gal[p].BlackHoleMass/Hubble_h * (HotGas/Hubble_h) * 10.;
else if(AGNRadioModeModel == 2)
{
//empirical (standard) accretion recipe - Eq. 10 in Croton 2006
AGNrate = AgnEfficiency / (UNITMASS_IN_G / UnitTime_in_s * SEC_PER_YEAR / SOLAR_MASS)
* (Gal[p].BlackHoleMass / 0.01) * pow3(Vvir / 200.0)
* ((HotGas / HotRadius * Rvir / Mvir) / 0.1);
}
else if(AGNRadioModeModel == 3 || AGNRadioModeModel == 4)
{
double x, lambda, temp, logZ, tot_metals;
tot_metals = metals_total(Gal[p].MetalsHotGas);
/* temp -> Temperature of the Gas in Kelvin, obtained from
* hidrostatic equilibrium KT=0.5*mu_p*(Vc)^2 assuming Vvir~Vc */
temp = 35.9 * Vvir * Vvir;
if(tot_metals > 0)
logZ = log10(tot_metals / HotGas);
else
logZ = -10.0;
lambda = get_metaldependent_cooling_rate(log10(temp), logZ);
x = PROTONMASS * BOLTZMANN * temp / lambda; // now this has units sec g/cm^3
x /= (UnitDensity_in_cgs * UnitTime_in_s); // now in internal units
/* Bondi-Hoyle accretion recipe -- efficiency = 0.15
* Eq. 29 in Croton 2006 */
if(AGNRadioModeModel == 3)
AGNrate = (2.5 * M_PI * G) * (0.75 * 0.6 * x) * Gal[p].BlackHoleMass * 0.15;
else if(AGNRadioModeModel == 4)
{
/* Cold cloud accretion recipe -- trigger: Rff = 50 Rdisk,
* and accretion rate = 0.01% cooling rate
* Eq. 25 in Croton 2006 */
FreeFallRadius = HotGas / (6.0 * 0.6 * x * Rvir * Vvir) / HotRadius * Rvir;
if(Gal[p].BlackHoleMass > 0.0 && FreeFallRadius < Gal[p].GasDiskRadius * 50.0)
AGNrate = 0.0001 * CoolingGas / dt;
else
AGNrate = 0.0;
}
}
/* Eddington rate */
/* Note that this assumes an efficiency of 50%
* - it ignores the e/(1-e) factor in L = e/(1-e) Mdot c^2 */
EDDrate = 1.3e48 * Gal[p].BlackHoleMass / (UnitEnergy_in_cgs / UnitTime_in_s) / 9e10;
/* accretion onto BH is always limited by the Eddington rate */
if(AGNrate > EDDrate)
AGNrate = EDDrate;
/* accreted mass onto black hole the value of dt puts an h factor into AGNaccreted as required for code units */
AGNaccreted = AGNrate * dt;
/* cannot accrete more mass than is available! */
if(AGNaccreted > HotGas)
AGNaccreted = HotGas;
/* coefficient to heat the cooling gas back to the virial temperature of the halo */
/* 1.34e5 = sqrt(2*eta*c^2), eta=0.1 (standard efficiency) and c in km/s
* Eqs. 11 & 12 in Croton 2006 */
AGNcoeff = (1.34e5 / Vvir) * (1.34e5 / Vvir);
/* cooling mass that can be suppressed from AGN heating */
AGNheating = AGNcoeff * AGNaccreted;
if(AGNRadioModeModel == 0 && Gal[p].Type==1)
{
if(dist < Gal[FoFCentralGal].Rvir)
{
if(AGNheating > (Gal[p].CoolingGas + Gal[FoFCentralGal].CoolingGas))
{
AGNheating = (Gal[p].CoolingGas + Gal[FoFCentralGal].CoolingGas);
AGNaccreted = (Gal[p].CoolingGas + Gal[FoFCentralGal].CoolingGas) / AGNcoeff;
}
if(AGNheating > Gal[p].CoolingGas)
LeftOverEnergy = AGNheating - Gal[p].CoolingGas;
}
}
else
if(AGNheating > Gal[p].CoolingGas)
AGNaccreted = Gal[p].CoolingGas / AGNcoeff;
/* limit heating to cooling rate */
if(AGNheating > Gal[p].CoolingGas)
AGNheating = Gal[p].CoolingGas;
/* accreted mass onto black hole */
Gal[p].BlackHoleMass += AGNaccreted; //ROB: transfer_mass functions should be used here
Gal[p].RadioAccretionRate += AGNaccreted / (dt*STEPS);
fraction=AGNaccreted/Gal[p].HotGas;
Gal[p].HotGas -= AGNaccreted;
Gal[p].MetalsHotGas = metals_add(Gal[p].MetalsHotGas,Gal[p].MetalsHotGas, -fraction);
#ifdef INDIVIDUAL_ELEMENTS
Gal[p].HotGas_elements = elements_add(Gal[p].HotGas_elements,Gal[p].HotGas_elements,-fraction);
#endif
#ifdef METALS_SELF
Gal[p].MetalsHotGasSelf = metals_add(Gal[p].MetalsHotGasSelf,Gal[p].MetalsHotGasSelf,-fraction);
#endif
}
else
AGNheating = 0.0;
Gal[p].CoolingGas -= AGNheating;
if(Gal[p].CoolingGas < 0.0)
Gal[p].CoolingGas = 0.0;
Gal[p].CoolingRate += Gal[p].CoolingGas / (dt*STEPS);
if(AGNRadioModeModel == 0 && LeftOverEnergy>0.)
{
Gal[FoFCentralGal].CoolingGas -= LeftOverEnergy;
if(Gal[FoFCentralGal].CoolingGas < 0.0)
Gal[FoFCentralGal].CoolingGas = 0.0;
else
Gal[FoFCentralGal].CoolingRate -= LeftOverEnergy / (dt*STEPS);
}
mass_checks("cooling_recipe #2.",p);
}
}
void compute_cooling(int p, double dt, int ngal)
{
double Vvir, Rvir, x, lambda, tcool, rcool, temp, tot_hotMass, tot_metals, HotRadius;
double coolingGas, logZ, rho_rcool, rho0;
mass_checks("cooling_recipe #1",p);
tot_hotMass = Gal[p].HotGas;
tot_metals = metals_total(Gal[p].MetalsHotGas);
if(tot_hotMass > 1.0e-6)
{
Vvir = Gal[p].Vvir;
Rvir = Gal[p].Rvir;
tcool = Rvir / Vvir; // tcool = t_dynamical = Rvir/Vvir
/* temp -> Temperature of the Gas in Kelvin, obtained from
* hidrostatic equilibrium KT=0.5*mu_p*(Vc)^2 assuming Vvir~Vc */
temp = 35.9 * Vvir * Vvir;
if (Gal[p].Type == 0)
HotRadius = Gal[p].Rvir;
else
HotRadius = Gal[p].HotRadius;
if(tot_metals > 0)
logZ = log10(tot_metals / tot_hotMass);
else
logZ = -10.0;
//eq. 3 and 4 Guo2010
lambda = get_metaldependent_cooling_rate(log10(temp), logZ);
x = PROTONMASS * BOLTZMANN * temp / lambda; // now this has units sec g/cm^3
x /= (UnitDensity_in_cgs * UnitTime_in_s); // now in internal units
rho_rcool = x / (0.28086 * tcool);
/* an isothermal density profile for the hot gas is assumed here */
rho0 = tot_hotMass / (4 * M_PI * HotRadius);
rcool = sqrt(rho0 / rho_rcool);
if (Gal[p].CoolingRadius < rcool)
Gal[p].CoolingRadius = rcool;
//if Hotradius is used, when galaxies become type 1's there will be a discontinuity in the cooling
if(rcool > Rvir) // INFALL DOMINATED REGIME
//coolingGas = tot_hotMass; - Delucia 2007
/*comes in to keep the continuity (Delucia2004) */
coolingGas = tot_hotMass / (HotRadius / Vvir) * dt;
else // HOT PHASE REGIME
/*coolingGas = (tot_hotMass / Rvir) * (rcool / tcool) * dt */
coolingGas = (tot_hotMass / HotRadius) * (rcool / tcool) * dt ;
//Photoionizing background
if (log10(temp) < 4.0)
coolingGas = 0.;
if(coolingGas > tot_hotMass)
coolingGas = tot_hotMass;
else if(coolingGas < 0.0)
coolingGas = 0.0;
}
else
{
coolingGas = 0.0;
}
Gal[p].CoolingGas = coolingGas;
mass_checks("cooling_recipe #1.5",p);
}
/** @brief Main recipe, calculates the fraction of cold gas turned into stars due
* to star formation; the fraction of mass instantaneously recycled and
* returned to the cold gas; the fraction of gas reheated from cold to hot,
* ejected from hot to external and returned from ejected to hot due to
* SN feedback. */
void starformation_and_feedback(int p, int centralgal, double time, double dt, int nstep)
{
/*! Variables: reff-Rdisk, tdyn=Rdisk/Vmax, strdot=Mstar_dot, stars=strdot*dt*/
double tdyn, strdot, stars, reheated_mass, ejected_mass, fac, cold_crit,
metallicitySF, CentralVvir, MergeCentralVvir, EjectVmax, EjectVvir,
SN_Energy, Reheat_Energy;
//standard star formation law (Croton2006, Delucia2007, Guo2010)
if(StarFormationRecipe == 0)
{
if(Gal[p].Type == 0)
tdyn = Gal[p].GasDiskRadius / Gal[p].Vmax;
else
tdyn = Gal[p].GasDiskRadius / Gal[p].InfallVmax;
if(Gal[p].Type == 0)
cold_crit = 0.19 * Gal[p].Vmax * Gal[p].GasDiskRadius;
else
cold_crit = 0.19 * Gal[p].InfallVmax * Gal[p].GasDiskRadius;
if(Gal[p].ColdGas > cold_crit)
strdot = SfrEfficiency * (Gal[p].ColdGas - cold_crit) / tdyn * pow(Gal[p].Vvir / SfrLawPivotVelocity, SfrLawSlope);
else
strdot = 0.0;
}
//No dependce on Tdyn
if(StarFormationRecipe == 1)
{
if(Gal[p].ColdGas > 1.e-7)
strdot = SfrEfficiency * (Gal[p].ColdGas) / (2.e-5) * pow(Gal[p].Vvir / SfrLawPivotVelocity, SfrLawSlope);
else
strdot = 0.0;
}
#ifdef H2FORMATION
/* use H2 formation model from Krumholz */
Not yet implemented
H2Mass=cal_H2(p);
strdot = SfrEfficiency * H2Mass / tdyn;
#endif
/*TODO - Note that Units of dynamical time are Mpc/Km/s - no conversion on dt needed
* be mentioned 3.06e19 to 3.15e19 */
stars = strdot * dt;
if(stars < 0.0)
terminate("***error stars<0.0***\n");
/* SN FEEDBACK RECIPES */
/* In Guo2010 type 1s can eject, reincorporate gas and get gas from their
* own satellites (is not sent to the type 0 galaxy as in Delucia2007),
* for gas flow computations:
* If satellite is inside Rvir of main halo, Vvir of main halo used
* If it is outside, the Vvir of its central subhalo is used. */
CentralVvir = Gal[centralgal].Vvir; // main halo Vvir
MergeCentralVvir = Gal[Gal[p].CentralGal].Vvir; //central subhalo Vvir
mass_checks("recipe_starform #0",p);
mass_checks("recipe_starform #0.1",centralgal);
/* Feedback depends on the circular velocity of the host halo
* Guo2010 - eq 18 & 19*/
if(FeedbackRecipe == 0) {
if (Gal[Gal[p].CentralGal].Type == 0)
reheated_mass = FeedbackReheatingEpsilon * stars*
(.5+1./pow(Gal[Gal[p].CentralGal].Vmax/ReheatPreVelocity,ReheatSlope));
else
reheated_mass = FeedbackReheatingEpsilon * stars*
(.5+1./pow(Gal[Gal[p].CentralGal].InfallVmax/ReheatPreVelocity,ReheatSlope));
}
//Make sure that the energy used in reheat does not exceed the SN energy (central subhalo Vvir used)
if (FeedbackRecipe == 0 || FeedbackRecipe == 1) {
if (reheated_mass * Gal[Gal[p].CentralGal].Vvir * Gal[Gal[p].CentralGal].Vvir > stars * (EtaSNcode * EnergySNcode))
reheated_mass = stars * (EtaSNcode * EnergySNcode) / (Gal[Gal[p].CentralGal].Vvir * Gal[Gal[p].CentralGal].Vvir);
}
/* cant use more cold gas than is available! so balance SF and feedback */
if((stars + reheated_mass) > Gal[p].ColdGas) {
fac = Gal[p].ColdGas / (stars + reheated_mass);
stars *= fac;
reheated_mass *= fac;
}
/* Determine ejection (for FeedbackRecipe 2 we have the dependence on Vmax)
* Guo2010 - eq 22
* Note that satellites can now retain gas and have their own gas cycle*/
if (Gal[Gal[p].CentralGal].Type == 0)
{
EjectVmax=Gal[centralgal].Vmax;
EjectVvir=Gal[centralgal].Vvir;// main halo Vvir
}
else
{
EjectVmax=Gal[Gal[p].CentralGal].InfallVmax;
EjectVvir=Gal[Gal[p].CentralGal].Vvir; //central subhalo Vvir
}
if(FeedbackRecipe == 0)
{
ejected_mass =
(FeedbackEjectionEfficiency* (EtaSNcode * EnergySNcode) * stars *
min(1./FeedbackEjectionEfficiency, .5+1/pow(EjectVmax/EjectPreVelocity,EjectSlope)) -
reheated_mass*EjectVvir*EjectVvir) /(EjectVvir*EjectVvir);
}
else if(FeedbackRecipe == 1)//the ejected material is assumed to have V_SN
{
SN_Energy = .5 * stars * (EtaSNcode * EnergySNcode);
Reheat_Energy = .5 * reheated_mass * EjectVvir * EjectVvir;
ejected_mass = (SN_Energy - Reheat_Energy)/(0.5 * FeedbackEjectionEfficiency*(EtaSNcode * EnergySNcode));
//if VSN^2<Vvir^2 nothing is ejected
if(FeedbackEjectionEfficiency*(EtaSNcode * EnergySNcode)<EjectVvir*EjectVvir)
ejected_mass =0.0;
}
// Finished calculating mass exchanges, so just check that none are negative
if (reheated_mass < 0.0) reheated_mass = 0.0;
if (ejected_mass < 0.0) ejected_mass = 0.0;
/* update the star formation rate */
#ifdef SAVE_MEMORY
/*Sfr=stars/(dt*steps)=strdot*dt/(dt*steps)=strdot/steps -> average over the STEPS*/
Gal[p].Sfr += stars / (dt * STEPS);
#else
for(outputbin = 0; outputbin < NOUT; outputbin++) {
if(Halo[halonr].SnapNum == ListOutputSnaps[outputbin]) {
Gal[p].Sfr[outputbin] += stars / (dt * STEPS);
break;
}
}
#endif
mass_checks("recipe_starform #1",p);
mass_checks("recipe_starform #1.1",centralgal);
/* update for star formation
* updates Mcold, StellarMass, MetalsMcold and MetalsStellarMass
* in Guo2010 case updates the stellar spin -> hardwired, not an option */
/* Store the value of the metallicity of the cold phase when SF occurs */
if (Gal[p].ColdGas > 0.)
#ifdef METALS
//metallicitySF=Gal[p].MetalsColdGas.type2/Gal[p].ColdGas;
metallicitySF= metals_total(Gal[p].MetalsColdGas)/Gal[p].ColdGas;
#else
metallicitySF=Gal[p].MetalsColdGas/Gal[p].ColdGas;
#endif
else
