void make_bulge_from_burst(int p)
{
int outputbin, j;
/* generate bulge */
transfer_stars(p,"Bulge",p,"Disk",1.);
/* update the star formation rate */
#ifdef SAVE_MEMORY
Gal[p].SfrBulge = Gal[p].Sfr;
#else
for(outputbin = 0; outputbin < NOUT; outputbin++)
Gal[p].SfrBulge[outputbin] += Gal[p].Sfr[outputbin];
#endif
#ifndef POST_PROCESS_MAGS
#ifdef OUTPUT_REST_MAGS
for(outputbin = 0; outputbin < NOUT; outputbin++) {
for(j = 0; j < NMAG; j++) {
Gal[p].LumBulge[j][outputbin] = Gal[p].Lum[j][outputbin];
Gal[p].YLumBulge[j][outputbin] = Gal[p].YLum[j][outputbin];
}
}
#endif
#ifdef COMPUTE_OBS_MAGS
for(outputbin = 0; outputbin < NOUT; outputbin++) {
for(j = 0; j < NMAG; j++) {
Gal[p].ObsLumBulge[j][outputbin] = Gal[p].ObsLum[j][outputbin];
Gal[p].ObsYLumBulge[j][outputbin] = Gal[p].ObsYLum[j][outputbin];
#ifdef OUTPUT_MOMAF_INPUTS
Gal[p].dObsLumBulge[j][outputbin] = Gal[p].dObsLum[j][outputbin];
Gal[p].dObsYLumBulge[j][outputbin] = Gal[p].dObsYLum[j][outputbin];
#endif
}
}
#endif
#endif //POST_PROCESS_MAGS
}
void disrupt(int p, int centralgal)
{
double rho_sat, rho_cen;
double cen_mass, r_sat, radius;
int outputbin, j, q;
/* If the main halo density at the pericentre (closest point in the orbit
* to the central galaxy)is larger than the satellite's density at the
* half mass radius, the satellite is completely disrupted. Note that since
* the satellite is a type 2 the only mass components remaining and
* contributing to the density are the cold gas and stellar mass. */
//TODO If we are passing in centralgal then we should not set it here
centralgal=Gal[p].CentralGal;
mass_checks("Top of disrupt",centralgal);
mass_checks("Top of disrupt",p);
/* Radius calculated at the peri-point */
radius=peri_radius(p, centralgal);
if (radius < 0) {
terminate("must be wrong \n");
}
/* Calculate the density of the main central halo at radius (the peri-centre).
* The tidal forces are caused by the dark matter of the main halo, hence Mvir
* is used. */
cen_mass=Gal[centralgal].Mvir*radius/Gal[centralgal].Rvir;
rho_cen=cen_mass/pow3(radius);
/* Calculate the density of the satellite's baryonic material */
if (Gal[p].DiskMass+Gal[p].BulgeMass>0) {
/* Calculate the rho according to the real geometry */
r_sat = sat_radius(p);
/* Or use radius at the mean radius of the stellar mass */
/* r_sat=(Gal[p].BulgeMass*Gal[p].BulgeSize+(Gal[p].StellarMass-Gal[p].BulgeMass)
* *Gal[p].StellarDiskRadius/3*1.68)
* /(Gal[p].StellarMass); */
/* to calculate the density */
//rho_sat=Gal[p].StellarMass/pow2(r_sat);
rho_sat=(Gal[p].DiskMass+Gal[p].BulgeMass+Gal[p].ColdGas)/pow3(r_sat);
}
else
rho_sat=0.0;
/* If density of the main halo is larger than that of the satellite baryonic
* component, complete and instantaneous disruption is assumed. Galaxy becomes
* a type 3 and all its material is transferred to the central galaxy. */
if (rho_cen > rho_sat) {
Gal[p].Type = 3;
#ifdef GALAXYTREE
q = Gal[Gal[p].CentralGal].FirstProgGal;
if (q >= 0) {
// add progenitors of Gal[p] to the list of progentitors of Gal[p].CentralGal
while (GalTree[q].NextProgGal >= 0)
q = GalTree[q].NextProgGal;
GalTree[q].NextProgGal = Gal[p].FirstProgGal;
if(GalTree[q].NextProgGal >= NGalTree)
{
printf("q=%d p=%d GalTree[q].NextProgGal=%d NGalTree=%d\n",
q, p, GalTree[q].NextProgGal, NGalTree);
terminate("problem");
}
}
if(q < 0)
terminate("this shouldn't happen");
// TODO if !(q>=0) shouldn't we set
// Gal[Gal[p].CentralGal].FirstProgGal to Gal[p].FirstProgGal ??
q = GalTree[q].NextProgGal;
if(q < 0)
terminate("inconsistency");
if(HaloGal[GalTree[q].HaloGalIndex].GalTreeIndex != q)
terminate("inconsistency");
HaloGal[GalTree[q].HaloGalIndex].DisruptOn = 1;
#endif
/* Put gas component to the central galaxy hot gas and stellar material into the ICM.
* Note that the staellite should have no extended components. */
// TODO Shouldn't the stars end up in the bulge? - this is a close merger
transfer_gas(centralgal,"Hot",p,"Cold",1.);
transfer_gas(centralgal,"Hot",p,"Hot",1.);
transfer_stars(centralgal,"ICM",p,"Disk",1.);
transfer_stars(centralgal,"ICM",p,"Bulge",1.);
/* Add satellite's luminosity into the luminosity of the ICL
* component of the central galaxy. */
#ifdef ICL
for(outputbin = 0; outputbin < NOUT; outputbin++) {
for(j = 0; j < NMAG; j++) {
#ifdef OUTPUT_REST_MAGS
Gal[centralgal].ICLLum[j][outputbin] += Gal[p].Lum[j][outputbin];
#endif
#ifdef COMPUTE_OBS_MAGS
Gal[centralgal].ObsICL[j][outputbin] += Gal[p].ObsLum[j][outputbin];
#endif
}
}
#endif
}
mass_checks("Bottom of disrupt",centralgal);
mass_checks("Bottom of disrupt",p);
}
void add_galaxies_together(int t, int p)
{
/** @brief All the components of the satellite galaxy are added to the
* correspondent component of the central galaxy. Cold gas spin
* is updated and a bulge is formed at the central galaxy, with
* the stars of the satellite if BulgeFormationInMinorMergersOn=1.
*
* TODO Even though galaxy p has been set to type 3 (ie a non-galaxy), it would
* make mass conservation more explicit to zero the properties of galaxy p after
* the merger.
* TODO Correct artificial diffusion of metals when BulgeFormationInMinorMergersOn=1. */
int outputbin, j;
float tspin[3],tmass,pmass;
/* t central, p satellite */
mass_checks("add_galaxies_together #0",p);
mass_checks("add_galaxies_together #0.1",t);
/* angular momentum transfer between gas*/
tmass= Gal[t].ColdGas;
pmass= Gal[p].ColdGas;
Gal[t].MergeSat +=(Gal[p].DiskMass+Gal[p].BulgeMass);
Gal[p].MergeSat=0.;
transfer_gas(t,"Cold",p,"Cold",1.);
transfer_gas(t,"Hot",p,"Hot",1.);
transfer_gas(t,"Ejected",p,"Ejected",1.); //TODO chose move to ejected or hot
if(BulgeFormationInMinorMergersOn)
transfer_stars(t,"Bulge",p,"Disk",1.);
else
transfer_stars(t,"Disk",p,"Disk",1.);
transfer_stars(t,"Bulge",p,"Bulge",1.);
transfer_stars(t,"ICM",p,"ICM",1.);
Gal[t].BlackHoleMass += Gal[p].BlackHoleMass;
Gal[p].BlackHoleMass=0.;
Gal[t].BlackHoleGas += Gal[p].BlackHoleGas;
Gal[p].BlackHoleGas=0.;
Gal[t].StarMerge += Gal[p].StarMerge;
Gal[p].StarMerge=0.;
mass_checks("add_galaxies_together #1",p);
mass_checks("add_galaxies_together #1.1",t);
/*update the gas spin*/
for(j=0;j<3;j++)
tspin[j]=Gal[t].GasSpin[j]*tmass+Gal[t].HaloSpin[j]*pmass;
if (Gal[t].ColdGas != 0)
for (j=0;j<3;j++)
Gal[t].GasSpin[j]=tspin[j]/(Gal[t].ColdGas);
#ifdef SAVE_MEMORY
Gal[t].Sfr += Gal[p].Sfr;
#else
for(outputbin = 0; outputbin < NOUT; outputbin++)
Gal[t].Sfr[outputbin] += Gal[p].Sfr[outputbin];
#endif
if(BulgeFormationInMinorMergersOn) {
#ifdef SAVE_MEMORY
Gal[t].SfrBulge += Gal[p].Sfr;
#else
for(outputbin = 0; outputbin < NOUT; outputbin++)
Gal[t].SfrBulge[outputbin] += Gal[p].Sfr[outputbin];
#endif
}
/* Add the black hole accretion rates. This makes little sense but is not
* used if the superior BlackHoleGrowth==1 switch is on. */
Gal[t].QuasarAccretionRate += Gal[p].QuasarAccretionRate;
Gal[t].RadioAccretionRate += Gal[p].RadioAccretionRate;
#ifndef POST_PROCESS_MAGS
/* Add the luminosities of the satellite and central galaxy */
#ifdef OUTPUT_REST_MAGS
for(outputbin = 0; outputbin < NOUT; outputbin++)
{
for(j = 0; j < NMAG; j++) {
Gal[t].Lum[j][outputbin] += Gal[p].Lum[j][outputbin];
Gal[t].YLum[j][outputbin] += Gal[p].YLum[j][outputbin];
#ifdef ICL
Gal[t].ICLLum[j][outputbin] += Gal[p].ICLLum[j][outputbin];
#endif
}
if(BulgeFormationInMinorMergersOn) {
for(j = 0; j < NMAG; j++) {
Gal[t].LumBulge[j][outputbin] += Gal[p].Lum[j][outputbin];
Gal[t].YLumBulge[j][outputbin] += Gal[p].YLum[j][outputbin];
}
}
else {
for(j = 0; j < NMAG; j++) {
Gal[t].LumBulge[j][outputbin] += Gal[p].LumBulge[j][outputbin];
Gal[t].YLumBulge[j][outputbin] += Gal[p].YLumBulge[j][outputbin];
}
}
Gal[t].MassWeightAge[outputbin] += Gal[p].MassWeightAge[outputbin];
}
#endif // OUTPUT_REST_MAGS
#ifdef COMPUTE_OBS_MAGS
for(outputbin = 0; outputbin < NOUT; outputbin++)
{
for(j = 0; j < NMAG; j++) {
Gal[t].ObsLum[j][outputbin] += Gal[p].ObsLum[j][outputbin];
Gal[t].ObsYLum[j][outputbin] += Gal[p].ObsYLum[j][outputbin];
#ifdef ICL
Gal[t].ObsICL[j][outputbin] += Gal[p].ObsICL[j][outputbin];
#endif
#ifdef OUTPUT_MOMAF_INPUTS
Gal[t].dObsLum[j][outputbin] += Gal[p].dObsLum[j][outputbin];
Gal[t].dObsYLum[j][outputbin] += Gal[p].dObsYLum[j][outputbin];
#endif
}
if(BulgeFormationInMinorMergersOn) {
for(j = 0; j < NMAG; j++) {
Gal[t].ObsLumBulge[j][outputbin] += Gal[p].ObsLum[j][outputbin];
Gal[t].ObsYLumBulge[j][outputbin] += Gal[p].ObsYLum[j][outputbin];
#ifdef OUTPUT_MOMAF_INPUTS
Gal[t].dObsLumBulge[j][outputbin] += Gal[p].dObsLum[j][outputbin];
Gal[t].dObsYLumBulge[j][outputbin] += Gal[p].dObsYLum[j][outputbin];
#endif
}
}
else
{
for(j = 0; j < NMAG; j++) {
Gal[t].ObsLumBulge[j][outputbin] += Gal[p].ObsLumBulge[j][outputbin];
Gal[t].ObsYLumBulge[j][outputbin] += Gal[p].ObsYLumBulge[j][outputbin];
#ifdef OUTPUT_MOMAF_INPUTS
Gal[t].dObsLumBulge[j][outputbin] += Gal[p].dObsLumBulge[j][outputbin];
Gal[t].dObsYLumBulge[j][outputbin] += Gal[p].dObsYLumBulge[j][outputbin];
#endif
}
}
}
#endif //COMPUTE_OBS_MAGS
#endif //POST_PROCESS_MAGS
}
/** @brief Checks for disk stability using the
* Mo, Mao & White (1998) criteria */
void check_disk_instability(int p)
{
double Mcrit, fraction, stars, diskmass;
/** @brief Calculates the stability of the stellar disk as discussed
* in Mo, Mao & White (1998). For unstable stars, the required
* amount is transfered to the bulge to make the disk stable again.
* Mass, metals and luminosities updated. After Guo2010 the bulge
* size is followed and needs to be updated.
* Eq 34 & 35 in Guo2010 are used. */
if(DiskInstabilityModel == 0)
{
/* check stellar disk -> eq 34 Guo2010*/
if (Gal[p].Type != 0)
Mcrit = Gal[p].InfallVmax * Gal[p].InfallVmax * Gal[p].StellarDiskRadius / G;
else
Mcrit = Gal[p].Vmax * Gal[p].Vmax * Gal[p].StellarDiskRadius / G;
diskmass = Gal[p].DiskMass;
stars = diskmass - Mcrit;
fraction = stars / diskmass;
}
else if (DiskInstabilityModel == 1)
stars = 0.;
/* add excess stars to the bulge */
if(stars > 0.0)
{
/* to calculate the bulge size */
update_bulge_from_disk(p,stars);
transfer_stars(p,"Bulge",p,"Disk",fraction);
if(BHGrowthInDiskInstabilityModel == 1)
if(Gal[p].ColdGas > 0.)
{
Gal[p].BlackHoleMass += Gal[p].ColdGas*fraction;
Gal[p].ColdGas -= Gal[p].ColdGas*fraction;
}
#ifndef POST_PROCESS_MAGS
double Lumdisk;
int outputbin, j;
#ifdef OUTPUT_REST_MAGS
for(outputbin = 0; outputbin < NOUT; outputbin++)
{
for(j = 0; j < NMAG; j++)
{
Lumdisk = Gal[p].Lum[j][outputbin]-Gal[p].LumBulge[j][outputbin];
Gal[p].LumBulge[j][outputbin] += fraction * Lumdisk;
Lumdisk = Gal[p].YLum[j][outputbin]-Gal[p].YLumBulge[j][outputbin];
Gal[p].YLumBulge[j][outputbin] += fraction * Lumdisk;
}
}
#endif
#ifdef COMPUTE_OBS_MAGS
for(outputbin = 0; outputbin < NOUT; outputbin++)
{
for(j = 0; j < NMAG; j++)
{
Lumdisk = Gal[p].ObsLum[j][outputbin]-Gal[p].ObsLumBulge[j][outputbin];
Gal[p].ObsLumBulge[j][outputbin] += fraction * Lumdisk;
Lumdisk = Gal[p].ObsYLum[j][outputbin]-Gal[p].ObsYLumBulge[j][outputbin];
Gal[p].ObsYLumBulge[j][outputbin] += fraction * Lumdisk;
#ifdef OUTPUT_MOMAF_INPUTS
Lumdisk = Gal[p].dObsLum[j][outputbin]-Gal[p].dObsLumBulge[j][outputbin];
Gal[p].dObsLumBulge[j][outputbin] += fraction * Lumdisk;
Lumdisk = Gal[p].dObsYLum[j][outputbin]-Gal[p].dObsYLumBulge[j][outputbin];
Gal[p].dObsYLumBulge[j][outputbin] += fraction * Lumdisk;
#endif
}
}
#endif
#endif
if ((Gal[p].BulgeMass > 1e-9 && Gal[p].BulgeSize == 0.0)||
(Gal[p].BulgeMass == 0.0 && Gal[p].BulgeSize >1e-9))
{
char sbuf[1000];
sprintf(sbuf, "bulgesize wrong in diskinstablility.c \n");
terminate(sbuf);
}
}// if(stars > 0.0)
}
