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main.c
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main.c
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/***************************************************************************
* Copyright (C) 2009 by Andreas H.W. Kuepper *
* akuepper@astro.uni-bonn.de *
* *
* This program is free software; you can redistribute it and/or modify *
* it under the terms of the GNU General Public License as published by *
* the Free Software Foundation; either version 2 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 General Public License *
* along with this program; if not, write to the *
* Free Software Foundation, Inc., *
* 59 Temple Place - Suite 330, Boston, MA 02111-1307, USA. *
***************************************************************************/
/***************************************************************************
* Compile using the command: cc -lm -o mcluster mcluster.c *
* or use the Makefile, i.e. type: make mcluster or make mcluster_sse *
***************************************************************************/
/***************************************************************************
* Main array with stellar parameters: *
* star[][0] = mass(t = epoch) *
* star[][1-3] = {x, y, z} *
* star[][4-6] = {vx, vy, vz} *
* star[][7] = mass(t = 0) *
* star[][8] = kstar, stellar type in (SSE/BSE) *
* star[][9] = epoch1, age within evolutionary phase (SSE/BSE) *
* star[][10] = ospin, spin of star (SSE/BSE) *
* star[][11] = rstar, radius of star (SSE/BSE) *
* star[][12] = lstar, luminosity (SSE/BSE) *
* star[][13] = epochstar, age of star (SSE/BSE) *
* star[][14] = Zstar, metallicity of star *
***************************************************************************/
#include<stdio.h>
#include<stdlib.h>
#include<math.h>
#include<time.h>
#include<string.h>
#include<sys/stat.h>
#include<getopt.h>
#ifdef GPU
#include <cuda.h>
#include <cuda_runtime.h>
#endif
#include "main.h"
//use OpenMP if not specified otherwise
#ifndef NOOMP
#include<omp.h>
#endif
int main (int argv, char **argc) {
/*******************
* Input variables *
*******************/
//Basic physical parameters
int N = 0; //Number of stars, Mcl will be set to 0 if specified!
double Mcl = 1000.0; //Total mass of the cluster, only used when N is set to 0, necessary for usage of maximum stellar mass relation of Weidner & Kroupa (2006)
int profile = 0; //Density profile; =0 Plummer model, =1 King model (based on king0.f by D.C. Heggie), =2 mass segregated Subr model (Subr et al. 2007), =3 2-dimensional EFF template (Elson, Fall & Freeman 1987) or Nuker template (Lauer et al. 1995), =-1 no density gradient
double W0 = 5.0; //King's W0 paramter [0.3-12.0]
double S = 0.0; //Fraction of mass segregation for profile; =0.0 unsegregated, =1.0 completely segregated (take maximally S=0.99 for profile=2)
double D = 3.0; //Fractal dimension; =3.0 unfractal, =2.6 2/8 fractal, =2.0 4/8 fractal, =1.6 6/8 fractal, (2^D children per parent, following Goodwin & Whitworth 2004);
double Q = 0.5; //Initial virial ratio; =0.5 virial equilibrium, <0.5 collapsing, >0.5 expanding
double Rh = 0.8; //Half-mass radius [pc], ignored if profile = 3, set =-1 for using Marks & Kroupa (2012) Mcl-Rh relation
double gamma[3] = {2.0, 0.0, 2.0}; //Power-law slopes of EFF/Nuker templates (outer slope, inner slope, transition); set gamma[1] = 0.0 and gamma[2] = 2.0 for EFF (profile = 3)
double a = 1.0; //Scale radius of EFF/Nuker template (profile = 3) [pc]
double Rmax = 100.0; //Cut-off radius for EFF/Nuker template (profile = 3) [pc]
double tcrit = 100.0; //Simulation time [N-body units (Myr in Nbody6 custom)]
int tf = 3; //Tidal field: =0 no tidal field, =1 Near-field approximation, =2 point-mass galaxy, =3 Allen & Santillan (1991) MW potential (or Sverre's version of it)
double RG[3] = {8500.0,0.0,0.0}; //Initial Galactic coordinates of the cluster [pc]
double VG[3] = {0.0,220.0,0.0}; //Initial velocity of the cluster [km/s]
//Mass function parameters
int mfunc = 1; //0 = single mass stars; 1 = use Kroupa (2001) mass function; 2 = use multi power law (based on mufu.c by L.Subr)
double single_mass = 1.0; //Stellar mass in case of single-mass cluster
double mlow = 0.08; //Lower mass limit for mfunc = 1 & mfunc = 4
double mup = 100.0; //Upper mass limit for mfunc = 1 & mfunc = 4
double alpha[MAX_AN] = {-1.35, -2.35, -2.7, 0.0, 0.0}; //alpha slopes for mfunc = 2
double mlim[MAX_MN] = {0.08, 0.5, 4.0, 100.0, 0.0, 0.0}; //mass limits for mfunc = 2
double alpha_L3 = 2.3; //alpha slope for mfunc = 4 (L3 mass function, Maschberger 2012)
double beta_L3 = 1.4; //beta slope for mfunc = 4
double mu_L3 = 0.2; //mu parameter for mfunc = 4
int weidner = 0; //Usage of Weidner & Kroupa (2006) relation for most massive star; =0 off, =1 on
int mloss = 3; //Stellar evolution; 0 = off, 3 = Eggleton, Tout & Hurley [KZ19]
int remnant = 1; //Use random kick velocity and present-day escape velocity to determine retention of compact remnants & evolved binary components (only for SSE/BSE version); =0 off, =1 on
double epoch = 0.0; //Age of the cluster, i.e. star burst has been ... Myr before [e.g. 1000.0, default = 0.0] [needs special compiling and SSE by Hurley, Pols & Tout]
double Z = 0.02; //Metallicity [0.0001-0.03, 0.02 = solar]
double FeH = -1.41; //Metallicity [Fe/H], only used when Z is set to 0
int prantzos = 0; //Usage of Prantzos (2007) relation for the life-times of stars. Set upper mass limit to Lifetime(mup) >= epoch
//Binary parameters
int nbin = 0; //Number of primordial binary systems
double fbin = 0.0; //Primordial binary fraction, number of binary systems = 0.5*N*fbin, only used when nbin is set to 0
int pairing = 3; //Pairing of binary components; 0= random pairing, 1= ordered pairing for components with masses M>msort, 2= random but separate pairing for components with masses m>Msort; 3= Use period distribution for M>msort from Sana et al. (2011,2012) and Oh et al. (2015).
double msort = 5.0; //Stars with masses > msort will be sorted and preferentially paired into binaries if pairing = 1
int adis = 3; //Semi-major axis distribution; 0= flat ranging from amin to amax, 1= based on Kroupa (1995) period distribution, 2= based on Duquennoy & Mayor (1991) period distribution, 3= based on Kroupa (1995) period distribution
int OBperiods = 2; //1: Use period distribution for massive binaries with M_primary > msort from Sana & Evans (2011); 2: Uniform distribution of mass ratio (0.1<q<1.0) for m>Msort and random pairing for remaining (Kiminki & Kobulnicky 2012; Sana et al., 2012; Kobulnicky et al. 2014; Oh, S., Kroupa, P., & Pflamm-Altenburg, J. (2015) period distribution for M>Msort (implemented by Long Wang)
double amin = 0.0001; //Minimum semi-major axis for adis = 0 [pc]
double amax = 0.01; //Maximum semi-major axis for adis = 0 [pc]
#ifdef SSE
int eigen = 0; //Use Kroupa (1995) eigenevolution for pre-main sequence short-period binaries; =0 off, =1 on [use either eigenevolution or BSE; BSE recommended when using SSE]
int BSE = 1; //Apply binary star evolution using BSE (Hurley, Tout & Pols 2002) =0 off, =1 on [use either eigenevolution or BSE; BSE recommended when using SSE]
#else
int eigen = 2; // 1. Use Kroupa (1995) eigenevolution for pre-main sequence short-period binaries; 2. Use modified eigenevolution from Belloni et al. (2017); 0. Off
int BSE = 0; //Apply binary star evolution using BSE (Hurley, Tout & Pols 2002) [needs special compiling and BSE]; =0 off, =1 on [use either eigenevolution or BSE; BSE recommended when using SSE]
#endif
//Gas parameters (only used for Nbody6 input)
double extmass = 0.0; //external Plummer (gas) sphere mass [Msun]
double extrad = 0.0; //external Plummer (gas) sphere scale factor [pc]
double extdecay = 0.0; //decay time for gas expulsion (set 0 for no decay) [Myr]
double extstart = 0.0; //delay time for start of gas expulsion [Myr]
//Code parameters
int code = 3; //Nbody version: =0 Nbody6, =1 Nbody4, =2 Nbody6 custom, =3 only create output list of stars, =4 Nbody7 (not yet fully functional), =5 Nbody6++GPU
unsigned int seed = 0; //Number seed for random number generator; =0 for randomization by local time
char *output = "test"; //Name of output files
double dtadj = 1.0; //DTADJ [N-body units (Myr in Nbody6 custom)], energy-check time step
double dtout = 1.0; //DELTAT [N-body units (Myr in Nbody6 custom)], output interval, must be multiple of DTADJ
double dtplot = 1.0; //DTPLOT [N-body units (Myr in Nbody6 custom)], output of HRdiagnostics, should be multiple of DTOUT, set to zero if output not desired
int gpu = 0; //Use of GPU, 0= off, 1= on
int regupdate = 0; //Update of regularization parameters during computation; 0 = off, 0 > on
int etaupdate = 0; //Update of ETAI & ETAR during computation; 0 = off, 0 > on
int esc = 2; //Removal of escapers; 0 = no removal, 1 = regular removal at 2*R_tide; 2 = removal and output in ESC
int units = 1; //Units of McLuster output; 0= Nbody-Units, 1= astrophysical units
//McLuster internal parameters
int match = 1; //Make cluster half-mass radius exactly match the expected/desired value; =0 off, =1 on (recommended)
int symmetry = 1; //Force spherical symmetry for fractal clusters; =0 off, =1 on (recommended)
int check = 0; //Make energy check at end of McLuster; =0 off, =1 on
int create_radial_profile = 1; //Creates a radial density profile and prints it to the screen; =0 off, =1 on
int create_cumulative_profile = 1; //Creates a radial cumulative profile and prints it to the screen; =0 off, =1 on
double Rgal = 10000.0; //Distance of cluster from sun for artificial CMD with observational errors [pc]
double Zsun = 0.02; //Solar metallicity
int NNBMAX_NBODY6 = 500; //Maximum number of neighbours allowed in NBODY6
double upper_IMF_limit = 150.0; //Maximum stellar mass allowed in McLuster [Msun]
int an = 0; //Counter for number of alpha slopes for mfunc = 2
int mn = 0; //Counter for number of mass limits for mfunc = 1, 2 & 4
int xn = 0; //Counter for components of galactocentric radius vector
int vn = 0; //Counter for components of cluster velocity vector
int xx = 0; //Counter for external potential input parameters
int gn = 0; //Counter for EFF/Nuker profile parameters
double extgas[4]; //Input array for external potential parameters
//SSE internal parameters (see Hurley, Pols & Tout 2000)
value1_.neta = 0.5; //Reimers mass-loss coefficent (neta*4x10^-13; 0.5 normally)
value1_.bwind = 0.0; //Binary enhanced mass loss parameter (inactive for single)
value1_.hewind = 1.0; //Helium star mass loss factor (1.0 normally)
value1_.mxns = 3.0; //Maximum NS mass (1.8, nsflag=0; 3.0, nsflag=1)
points_.pts1 = 0.05; //Time-step parameter in evolution phase: MS (0.05)
points_.pts2 = 0.01; //Time-step parameter in evolution phase: GB, CHeB, AGB, HeGB (0.01)
points_.pts3 = 0.02; //Time-step parameter in evolution phase: HG, HeMS (0.02)
value4_.sigma = 190.0; //Kick velocities
value4_.bhflag = 1; //bhflag > 0 allows velocity kick at BH formation
//BSE internal parameters (see Hurley, Pols & Tout 2002)
flags_.ceflag = 0; //ceflag > 0 activates spin-energy correction in common-envelope (0) #defunct#
flags_.tflag = 1; //tflag > 0 activates tidal circularisation (1)
flags_.ifflag = 0; //ifflag > 0 uses WD IFMR of HPE, 1995, MNRAS, 272, 800 (0)
flags_.nsflag = 1; //nsflag > 0 takes NS/BH mass from Belczynski et al. 2002, ApJ, 572, 407 (1)
flags_.wdflag = 1; //wdflag > 0 uses modified-Mestel cooling for WDs (0)
value5_.beta = 1.0/8.0; //beta is wind velocity factor: proportional to vwind**2 (1/8)
value5_.xi = 1.0; //xi is the wind accretion efficiency factor (1.0)
value5_.acc2 = 3.0/2.0; //acc2 is the Bondi-Hoyle wind accretion factor (3/2)
value5_.epsnov = 0.001; //epsnov is the fraction of accreted matter retained in nova eruption (0.001)
value5_.eddfac = 1.0; //eddfac is Eddington limit factor for mass transfer (1.0)
value5_.gamma = -1.0; //gamma is the angular momentum factor for mass lost during Roche (-1.0)
value2_.alpha1 = 1.0; //alpha1 is the common-envelope efficiency parameter (1.0)
value2_.lambda = 0.5; //lambda is the binding energy factor for common envelope evolution (0.5)
//Command line input
int option;
while ((option = getopt(argv, argc, "N:M:P:W:R:r:c:g:S:D:T:Q:C:A:O:G:o:f:a:m:B:b:p:s:t:e:Z:X:x:V:u:h:?")) != -1) switch (option)
{
case 'N': N = atoi(optarg); Mcl = 0.0; break;
case 'M': Mcl = atof(optarg); N = 0; break;
case 'P': profile = atoi(optarg); break;
case 'W': W0 = atof(optarg); break;
case 'R': Rh = atof(optarg); break;
case 'r': a = atof(optarg); break;
case 'c': Rmax = atof(optarg); break;
case 'g':
if (gn < 3) { gamma[gn] = atof(optarg); gn++; break; }
case 'S': S = atof(optarg); break;
case 'D': D = atof(optarg); break;
case 'T': tcrit = atof(optarg); break;
case 'Q': Q = atof(optarg); break;
case 'C': code = atoi(optarg); break;
case 'A': dtadj = atof(optarg); break;
case 'O': dtout = atof(optarg); break;
case 'G': gpu = atoi(optarg); break;
case 'o': output = optarg; break;
case 'f': mfunc = atoi(optarg); break;
case 'a' :
if (an < MAX_AN) {
alpha[an] = atof(optarg);
if (an == 0) alpha_L3 = atof(optarg);
if (an == 1) beta_L3 = atof(optarg);
if (an == 2) mu_L3 = atof(optarg);
an++;
break;
} else { printf("\nError: Number of alphas exceeded maximum limit of %d\n", MAX_AN); return 1; }
case 'm' :
if (mn < MAX_MN) {
mlim[mn] = atof(optarg);
if (mn == 0) mlow = atof(optarg);
if (mn == MAX_MN-1) mup = atof(optarg);
mn++;
break;
} else { printf("\nError: Number of mass params exceded maximum limit of %d\n", MAX_MN); return 1; }
case 'B': nbin = atoi(optarg); break;
case 'b': fbin = atof(optarg); break;
case 'p': pairing = atoi(optarg); break;
case 's': seed = atoi(optarg); break;
case 't': tf = atoi(optarg); break;
case 'e': epoch = atof(optarg); break;
case 'Z': Z = atof(optarg); break;
case 'X' :
if (xn < 3) { RG[xn] = atof(optarg); xn++; break; }
case 'V' :
if (vn < 3) { VG[vn] = atof(optarg); vn++; break; }
case 'x' :
if (xx < 4) { extgas[xx] = atof(optarg); xx++; break; }
case 'u': units = atoi(optarg); break;
case ':':
case 'h': help(msort); return 1;
case '?': help(msort); return 1;
};
if (mn-1 > 0) mup = mlim[mn-1];
//print summary of input parameters to .info file
info(output, N, Mcl, profile, W0, S, D, Q, Rh, gamma, a, Rmax, tcrit, tf, RG, VG, mfunc, single_mass, mlow, mup, alpha, mlim, alpha_L3, beta_L3, mu_L3, weidner, mloss, remnant, epoch, Z, prantzos, nbin, fbin, pairing, msort, adis, amin, amax, eigen, BSE, extmass, extrad, extdecay, extstart, code, seed, dtadj, dtout, dtplot, gpu, regupdate, etaupdate, esc, units, match, symmetry, OBperiods);
/*********
* Start *
*********/
printf("\n-----START---- \n");
#ifdef NOOMP
clock_t t1, t2;
t1 = clock(); //start stop-watch
#else
double t1, t2;
#pragma omp parallel
{
if (omp_get_thread_num() == 0)
if (omp_get_num_threads() > 1) printf("\n\nUsing OpenMP with %d threads\n", omp_get_num_threads());
t1 = omp_get_wtime(); //start stop-watch
}
#endif
if (seed) srand48(seed); //initialize random number generator by seed
else {
seed = (unsigned) time(NULL); //initialize random number generator by local time
seed %= 100000;
srand48(seed);
}
printf ("\n\nRandom seed = %i\n\n\n", seed);
if (seed) value3_.idum = seed; //idum is the random number seed used in the kick routine.
else value3_.idum = 10000000.0*drand48();
int i,j;
double M; //Total mass [M_sun]
double mmean; //Mean stellar mass [M_sun]
int NNBMAX; //Maximum neighbour number (Nbody6 only)
double RS0; //Initial radius of neighbour sphere [pc], Nbody6 only
double rtide; //Tidal radius [pc]
double omega; //Angular velocity of cluster around the galaxy
double rvir; //Virial radius [pc]
double cmr[7]; //For CoM correction
double rking, rplummer; //King-, Plummer radius
double MMAX; //most massive star
double tscale; //time-scale factor
double ekin = 0.0; //kinetic energy
double epot = 0.0; //potential energy
double sigma = 0.0; //velocity dispersion
int bin; //KZ(22) parameter (binaries yes/no)
int sse; //(evolved stellar population yes/no)
double submass[MAX_AN], subcount[MAX_AN], norm[MAX_AN], N_tmp, M_tmp; //mass function parameters for mfunc = 2
double Rh2D, Rh3D; //actual 2D/3D half-mass radius of the model
if (profile == 3) Rh = a; //set half-mass radius temporarily to scale radius for computation of escape velocity
if ((Mcl) && (N)) {
printf("\nWARNING: specify either Mcl (-M) or N (-N)!\n\n");
exit (1);
} else if ((!Mcl) && (mfunc == 3)) {
printf("\nWARNING: specify Mcl (-M) when using optimal sampling (-f 3)!\n\n");
exit (1);
}
if (xx > 0) {
if ((xx == 4) && (extgas[2])) {
extmass = extgas[0];
extrad = extgas[1];
extdecay = extgas[2];
extstart = extgas[3];
} else {
printf("\nWARNING: Insufficient or incorrect parameters specified for external Plummer potential!\n\n");
exit (1);
}
}
/***********************
* Generate star array *
***********************/
int columns = 15;
const int NMAX = N*2>1500000?N*2:1500000; //Maximum number of stars & orbits allowed in McLuster
double **star;
star = (double **)calloc(NMAX,sizeof(double *));
for (j=0;j<NMAX;j++){
star[j] = (double *)calloc(columns,sizeof(double));
if (star[j] == NULL) {
printf("\nMemory allocation failed!\n");
return 0;
}
}
/*******************************************
* Evaluate Z from [Fe/H] if Z is set to 0 *
*******************************************/
if (!Z) {
Z = pow(10.0, 0.977*FeH)*Zsun; //Bertelli, Bressan, Chiosi, Fagotto, Nasi, 1994, A&AS, 106, 275
printf("\nUsing Bertelli et al. (1994) relation to convert FeH = %.3f into Z = %.3f\n", FeH, Z);
}
/**********************************
* Calculate maximum stellar mass *
**********************************/
if (mfunc == 3) weidner = 1; //always use Weidner relation when using optimal sampling!
if (!N && weidner && mfunc) {
mup = upper_IMF_limit;
printf("\nUsing maximum stellar mass-cluster mass relation for upper stellar mass limit\n");
printf("\n(Weidner & Kroupa 2006, Pflamm-Altenburg & Kroupa 2007)\n");
//analytic fit to the observational data from Pflamm-Altenburg & Kroupa (2007), implementation by M. Kruckow
MMAX = pow(10,2.56*log10(Mcl)*pow(pow(3.82,9.17)+pow(log10(Mcl),9.17),-1/9.17)-0.38);
/*
//three-part power-law fit to the observational data
if (Mcl < 1000.0) {
MMAX = (log10(Mcl)*0.540563175) - 0.14120167;
MMAX = pow(10.0,MMAX);
} else if (Mcl < 3300.0) {
MMAX = (log10(Mcl)*0.19186051) + 0.9058611;
MMAX = pow(10.0,MMAX);
} else {
MMAX = (log10(Mcl)*0.360268003) + 0.313342031;
MMAX = pow(10.0,MMAX);
}*/
} else {
MMAX = mup;
}
if (mfunc && epoch && prantzos) {
printf("\nUsing Prantzos (2007) relation to reduce upper mass limit to Lifetime(mup) > epoch\n");
while (Lifetime(MMAX) < sqrt(pow(epoch,2))) {
MMAX -= 0.01;
}
}
/*******************
* Generate masses *
*******************/
printf("\n\n-----GENERATE MASSES----- \n");
//This loop has to be called multiple times with different N (or Mcl), Z and epoch in order to create multiple stellar populations
//make sure that epoch and Z are stored together with the stars, then concatenate all arrays
//for now, all Z and epochs are the same, i.e. a single stellar population
if (mfunc == 1) {
printf("\nMaximum stellar mass set to: %.2f\n", MMAX);
generate_m1(&N, star, mlow, mup, &M, &mmean, MMAX, Mcl, epoch, Z, Rh, remnant);
} else if (mfunc == 2) {
if (mn) {
for (i = mn+1; i < MAX_MN; i++) mlim[i] = 0.0;
} else {
for (i=0; i<MAX_MN; i++) {
if (mlim[i]) mn++;
}
}
if (an) {
for (i = an+1; i < MAX_AN; i++) alpha[i] = 0.0;
} else {
for (i=0; i<MAX_AN; i++) {
if (alpha[i]) an++;
}
}
if (an >= mn) an = mn - 1;
mn = an + 1;
if (!mn){
printf("\nError: at least one mass limit has to be specified\n");
return 1;
} else if (mn == 1) {
single_mass = mlim[0];
printf("\nSetting stellar masses to %g solar mass\n",single_mass);
if (!N) N = Mcl/single_mass;
for (j=0;j<N;j++) star[j][0] = 1.0/N;
mmean = single_mass;
M = N*mmean;
printf("\nM = %g\n", M);
} else {
printf("\nMaximum stellar mass set to: %.2f\n",MMAX);
norm[an-1] = 1.; //normalization factor of integral
N_tmp = subcount[an-1] = subint(mlim[an-1], mlim[an], alpha[an-1] + 1.); //integrated number of stars in interval [mlim[an-1]:mlim[an]]
M_tmp = submass[an-1] = subint(mlim[an-1], mlim[an], alpha[an-1] + 2.); //integrated mass of stars in interval [mlim[an-1]:mlim[an]]
for (i = an - 2; i >= 0; i--) {
norm[i] = norm[i+1] * pow(mlim[i+1], alpha[i+1] - alpha[i]);
subcount[i] = norm[i] * subint(mlim[i], mlim[i+1], alpha[i] + 1.);
N_tmp += subcount[i];
submass[i] = norm[i] * subint(mlim[i], mlim[i+1], alpha[i] + 2.);
M_tmp += submass[i];
}
generate_m2(an, mlim, alpha, Mcl, M_tmp, subcount, &N, &mmean, &M, star, MMAX, epoch, Z, Rh, remnant);
}
} else if (mfunc == 3) {
printf("\nMaximum stellar mass set to: %.2f\n",MMAX);
generate_m3(&N, star, mlow, mup, &M, &mmean, MMAX, Mcl);
randomize(star, N);
} else if (mfunc == 4) {
printf("\nMaximum stellar mass set to: %.2f\n", MMAX);
printf("\nUsing L3 IMF (Maschberger 2012)\n");
generate_m4(&N, star, alpha_L3, beta_L3, mu_L3, mlow, mup, &M, &mmean, MMAX, Mcl, epoch, Z, Rh, remnant);
} else {
printf("\nSetting stellar masses to %.1f solar mass\n", single_mass);
if (!N) N = Mcl/single_mass;
for (j=0;j<N;j++) {
star[j][0] = single_mass;
star[j][7] = single_mass;
star[j][8] = 0;
star[j][9] = 0.0;
star[j][10] = 0.0;
star[j][11] = 0.0;
star[j][12] = 0.0;
star[j][13] = 0.0;
star[j][14] = 0.0;
}
mmean = single_mass;
M = N*mmean;
printf("\nM = %g\n", M);
mloss = 0;
}
//set all stars to the same metallicity and age for now
double epochstar, zstar;
epochstar = 0.0; //age compared to the oldest stars in the cluster [Myr]
zstar = Z;
for (j=0;j<N;j++) {
star[j][13] = epochstar;
star[j][14] = zstar;
}
//Pair binary masses and convert to centre-of-mass particles
int Nstars;
if (!nbin) nbin = 0.5*N*fbin;
double **mbin; //component mass & stellar evol parameter array
mbin = (double **)calloc(nbin,sizeof(double *));
for (j=0;j<nbin;j++){
mbin[j] = (double *)calloc(20,sizeof(double));
if (mbin[j] == NULL) {
printf("\nMemory allocation failed!\n");
return 0;
}
}
Nstars = N;
if (nbin) {
printf("\nPreparing binary components.\n");
//Specify component pairing
if (pairing) {
if (pairing == 1) printf("\nApplying ordered pairing for stars with masses > %.1f Msun.\n",msort);
else if (pairing == 2) printf("\nApplying random pairing for stars with masses > %.1f Msun.\n",msort);
else if (pairing == 3) printf("\nApplying Sana et al. (2012) mass atio distribution for stars with masses > %.1f Msun.\n",msort);
order(star, N, M, msort, pairing);
} else {
randomize(star, N);
printf("\nApplying random pairing.\n");
}
N -= nbin;
for (j=0;j<nbin;j++) {
mbin[j][0] = star[2*j][0]+star[2*j+1][0]; //system mass
mbin[j][1] = star[2*j][0]; //primary mass
mbin[j][2] = star[2*j+1][0]; //secondary mass
mbin[j][3] = star[2*j][7]; //primary m0
mbin[j][4] = star[2*j][8]; //primary kw
mbin[j][5] = star[2*j][9]; //primary epoch1
mbin[j][6] = star[2*j][10]; //primary spin
mbin[j][7] = star[2*j][11]; //primary r
mbin[j][8] = star[2*j][12]; //primary lum
mbin[j][9] = star[2*j+1][7]; //secondary m0
mbin[j][10] = star[2*j+1][8]; //secondary kw
mbin[j][11] = star[2*j+1][9]; //secondary epoch1
mbin[j][12] = star[2*j+1][10]; //secondary spin
mbin[j][13] = star[2*j+1][11]; //secondary r
mbin[j][14] = star[2*j+1][12]; //secondary lum
mbin[j][15] = 1000+j; //identifier
mbin[j][16] = star[2*j][13]; //primary epochstar
mbin[j][17] = star[2*j+1][13]; //secondary epochstar
mbin[j][18] = star[2*j][14]; //primary zstar
mbin[j][19] = star[2*j+1][14]; //secondary zstar
star[2*j][0] += star[2*j+1][0]; //system mass
star[2*j+1][0] = 0.0;
star[2*j][7] = 1000+j; //identifier
star[2*j+1][7] = 0.0; //identifier
star[2*j][12] += star[2*j+1][12]; //system luminosity
star[2*j+1][12] = 0.0;
}
order(star, Nstars, M, 0.0, 0);
randomize(star, N);
}
//prepare mass segregation
double mlowest = MMAX; //search lowest mass star
double mhighest = 0; //search highest mass star
double mmeancom = 0.0;
for (i=0;i<N;i++) {
star[i][0] /= M; //scale masses to Nbody units
mmeancom += star[i][0];
if (star[i][0] < mlowest) mlowest = star[i][0];
if (star[i][0] > mhighest) mhighest = star[i][0];
}
mmeancom /= N;
int Nseg = ceil(N*mmeancom/mlowest); //number of necessary pos & vel pairs for Baumgardt et al. (2008) mass segregation routine
int Nunseg = N;
double *Mcum;
Mcum = (double *)calloc(N,sizeof(double));
if ((S) && !(profile == 2)) {//sort masses when mass segregation parameter > 0
printf("\nApplying mass segregation with S = %f\n",S);
segregate(star, N, S);
for (i=0;i<N;i++) {//calculate cumulative mass function Mcum
Mcum[i] = 0.0;
for (j=0;j<=i;j++) Mcum[i] = Mcum[i] + star[j][0];
}
N = Nseg;
}
/*************************************
* Generate positions and velocities *
*************************************/
printf("\n\n-----GENERATE POSITIONS & VELOCITIES----- \n");
//calculate half-mass radius according to Marks & Kroupa 2012 if Rh is set to -1
if ((Rh == -1) && (Mcl)) {
Rh = 0.1*pow(Mcl,0.13); //Marks & Kroupa (2012), implementation by M. Kruckow
printf("\nUsing Marks & Kroupa (2012) relation to derive half-mass radius from cluster mass: %g (pc)\n", Rh);
}
//evaluate approximate tidal radius assuming circular orbit
if (tf == 3) {
//in the case of Allen & Santillan potential, assume kappa = 1.4omega (eq. 9 in Kuepper et al. 2010)
omega = sqrt(VG[0]*VG[0]+VG[1]*VG[1]+VG[2]*VG[2])/sqrt(RG[0]*RG[0]+RG[1]*RG[1]+RG[2]*RG[2]);
rtide = pow(G*M/(2.0*omega*omega),1.0/3.0);
} else if (!tf) {
rtide = 1.0E5;
} else if ((tf == 1) && (code == 0 || code == 4 || code == 5)) {
//in case of Sverre's Nbody6 standard tidal field
rtide = pow(1.0*M/(3.0*M1pointmass),1.0/3.0)*8000.0;
} else {
//in the case of a point mass potential or near field approximation
rtide = pow(1.0*M/(3.0*M1pointmass),1.0/3.0)*sqrt(RG[0]*RG[0]+RG[1]*RG[1]+RG[2]*RG[2]);
}
printf("\nApproximate tidal radius: %g (pc)\n", rtide);
//generate scaled pos & vel, postpone scaling for Plummer and King in case of mass segregation
double rhtemp, rvirtemp;
if (profile == 1) {
printf("\nGenerating King model with parameters: N = %i\t W0 = %g\t Rh = %.3f\t D = %.2f\n",N, W0, Rh, D);
generate_king(N, W0, star, &rvirtemp, &rhtemp, &rking, D, symmetry);
} else if (profile == 2) {
N = Nunseg;
printf("\nGenerating segregated Subr model with parameters: N = %i\t S = %g\t Rh = %.3f\n",N, S, Rh);
rvir = Rh/0.76857063065978; //(value provided by L. Subr)
generate_subr(N, S, star, rtide, rvir);
printf ("\nrvir = %.5f\t rh = %.5f\t rtide = %.5f (pc)\n", rvir, Rh, rtide);
} else if (profile == 3) {
if (gamma[1] == 0.0 && gamma[2] == 2.0) printf("\nGenerating EFF model with parameters: N = %i\t a = %.1f\t gamma = %.3f\t Rmax = %.1f\t D = %.2f\n",N, a, gamma[0], Rmax, D);
else printf("\nGenerating Nuker model with parameters: N = %i\t a = %.1f\t gamma (outer) = %.3f\t gamma (inner) = %.3f\t transition = %.3f\t Rmax = %.1f\t D = %.2f\n",N, a, gamma[0],gamma[1],gamma[2], Rmax, D);
double p[6];
p[1] = 1.0; //rho0, will be scaled according to Rmax and Mtot
p[2] = a;//scale radius
p[3] = gamma[0];//outer power-law slope (>0.5)
p[4] = gamma[1];//inner power-law slope (0.0 for EFF template)
p[5] = gamma[2];//transition parameter (2.0 for EFF template)
generate_profile(N, star, Rmax, M, p, &Rh, D, symmetry);
printf("\nRh = %.1f pc\n", Rh);
} else if (profile == -1) {
printf("\nGenerating fractal distribution with parameters: N = %i\t Rh = %.3f\t D = %.2f\n", N, Rh, D);
fractalize(D, N, star, 0, symmetry);
rvir = Rh;
} else {
printf("\nGenerating Plummer model with parameters: N = %i\t Rh = %.3f\t D = %.2f\n", N, Rh, D);
rvir = Rh/0.772764;
rplummer = Rh/1.305;
generate_plummer(N, star, rtide, rvir, D, symmetry);
}
//Apply Baumgardt et al. (2008) mass segregation
if (!(profile == 2) && (S)) {
double **m_temp;
m_temp = (double **)calloc(Nunseg,sizeof(double *));
for (j=0;j<Nunseg;j++){
m_temp[j] = (double *)calloc(9,sizeof(double));
if (m_temp[j] == NULL) {
printf("\nMemory allocation failed!\n");
return 0;
}
}
for (i=0;i<Nunseg;i++) {//temporarily store the masses & stellar evol parameters
m_temp[i][0] = star[i][0];
m_temp[i][1] = star[i][7];
m_temp[i][2] = star[i][8];
m_temp[i][3] = star[i][9];
m_temp[i][4] = star[i][10];
m_temp[i][5] = star[i][11];
m_temp[i][6] = star[i][12];
m_temp[i][7] = star[i][13];
m_temp[i][8] = star[i][14];
}
printf("\nOrdering orbits by energy.\n");
energy_order(star, N, Nstars);
int nlow, nhigh, nrandom;
for (i=0;i<Nunseg;i++) {
nhigh = Nseg*Mcum[i];
if (i) {
nlow = Nseg*Mcum[i-1];
} else {
nlow = 0;
}
nrandom = (nhigh-nlow)*drand48()+nlow;
star[i][0] = m_temp[i][0];
star[i][1] = star[nrandom][1];
star[i][2] = star[nrandom][2];
star[i][3] = star[nrandom][3];
star[i][4] = star[nrandom][4];
star[i][5] = star[nrandom][5];
star[i][6] = star[nrandom][6];
star[i][7] = m_temp[i][1];
star[i][8] = m_temp[i][2];
star[i][9] = m_temp[i][3];
star[i][10] = m_temp[i][4];
star[i][11] = m_temp[i][5];
star[i][12] = m_temp[i][6];
star[i][13] = m_temp[i][7];
star[i][14] = m_temp[i][8];
}
for (j=0;j<Nunseg;j++) free (m_temp[j]);
free(m_temp);
N = Nunseg;
}
//CoM correction
printf("\nApplying centre-of-mass correction.\n");
for (j=0; j<7; j++) cmr[j] = 0.0;
for (j=0; j<N; j++) {
for (i=1;i<7;i++)
cmr[i] += star[j][0]*star[j][i];
}
for (j=0; j<N; j++) {
for (i=1;i<7;i++)
star[j][i] -= cmr[i];
}
//apply scaling to Nbody-units
if (profile == 0) {
printf("\nRe-scaling of orbits (dt ~ N^2!)\n");
double ke = 0.0;
double pe = 0.0;
double sx, sv, r2;
#ifdef GPU
gpupot(N,star,&pe);
#ifndef NOOMP
#pragma omp parallel shared(N, star) private(i)
{
#pragma omp for reduction(+: ke) schedule(dynamic)
#endif
for (i=0;i<N;i++) {
ke += star[i][0]*(pow(star[i][4],2)+pow(star[i][5],2)+pow(star[i][6],2));
}
#ifndef NOOMP
}
#endif
// printf("PE_GPU %lg ke %lg\n",pe,ke);
#else
#ifndef NOOMP
#pragma omp parallel shared(N, star) private(i, j, r2)
{
#pragma omp for reduction(+: pe, ke) schedule(dynamic)
#endif
for (i=0;i<N;i++) {
if (i) {
for (j=0;j<i-1;j++) {
r2 = (star[i][1]-star[j][1])*(star[i][1]-star[j][1]) + (star[i][2]-star[j][2])*(star[i][2]-star[j][2]) +(star[i][3]-star[j][3])*(star[i][3]-star[j][3]) ;
pe -= star[i][0]*star[j][0]/sqrt(r2);
}
}
ke += star[i][0]*(pow(star[i][4],2)+pow(star[i][5],2)+pow(star[i][6],2));
}
#ifndef NOOMP
}
#endif
// printf("PE_HOST %lg ke %lg\n",pe,ke);
#endif
rvir = -GNBODY*pow(MNBODY,2)/(2.0*pe);
sx = 1.0/rvir;
ke *= 0.5;
sv = sqrt(4.0*ke);
for (i=0;i<N;i++) {
star[i][1] *= sx;
star[i][2] *= sx;
star[i][3] *= sx;
star[i][4] /= sv;
star[i][5] /= sv;
star[i][6] /= sv;
}
ke = 0;
for (i=0;i<N;i++) {
ke += M*star[i][0]*(pow(star[i][4],2)+pow(star[i][5],2)+pow(star[i][6],2));
}
ke /= 0.5*N;
printf("Dynamical temperature of centre-of-mass particles kT = %lf\n\n",ke);
//make half-mass radius of the system match the desired one
radial_profile(star, N, rvir, M, 0, 0, code, &NNBMAX, &RS0, &Rh2D, &Rh3D, NNBMAX_NBODY6);
if (match) {
printf("\nmeasuring half-mass radius: %.7f \t %.7f (should/is)\nand correcting for this factor\n",Rh, Rh3D);
rvir = rvir *Rh/Rh3D;
}
printf ("\nrvir = %.5f\t rh = %.5f\t rplummer = %.5f\t rtide = %.5f (pc)\n", rvir, Rh, rplummer, rtide);
} else if ((profile == 1) || (profile == 3) || (profile == -1)) {
printf("\nRe-scaling of orbits (dt ~ N^2!)\n");
double pe = 0.0;
double ke = 0.0;
double r2, vscale;
#ifdef GPU
gpupot(N,star,&pe);
#ifndef NOOMP
#pragma omp parallel shared(N, star) private(i)
{
#pragma omp for reduction(+: ke) schedule(dynamic)
#endif
for (i=0;i<N;i++) {
ke += star[i][0]*(pow(star[i][4],2)+pow(star[i][5],2)+pow(star[i][6],2));
}
#ifndef NOOMP
}
#endif
// printf("PE_GPU %lg ke %lg\n",pe,ke);
#else
#ifndef NOOMP
#pragma omp parallel shared(N, star) private(i, j, r2)
{
#pragma omp for reduction(+: pe, ke) schedule(dynamic)
#endif
for (i=0;i<N;i++) {
for (j=0;j<i-1;j++) {
r2 = (star[i][1]-star[j][1])*(star[i][1]-star[j][1]) + (star[i][2]-star[j][2])*(star[i][2]-star[j][2]) +(star[i][3]-star[j][3])*(star[i][3]-star[j][3]) ;
pe -= star[i][0]*star[j][0]/sqrt(r2);
}
ke += star[i][0]*(pow(star[i][4],2)+pow(star[i][5],2)+pow(star[i][6],2));
}
#ifndef NOOMP
}
#endif
// printf("PE_HOST %lg ke %lg\n",pe,ke);
#endif
ke *= 0.5;
rvir = -GNBODY*pow(MNBODY,2)/(2.0*pe);
vscale = sqrt(4.0*ke);
ke = 0;
for (i=0;i<N;i++) {
for (j=0;j<3;j++) {
star[i][j+1] /= rvir;
star[i][j+4] /= vscale;
}
ke += M*star[i][0]*(pow(star[i][4],2)+pow(star[i][5],2)+pow(star[i][6],2));
}
ke /= 0.5*N;
printf("Dynamical temperature of centre-of-mass particles kT = %lf\n\n",ke);
//make half-mass radius of the system match the desired one
radial_profile(star, N, rvir, M, 0, 0, code, &NNBMAX, &RS0, &Rh2D, &Rh3D, NNBMAX_NBODY6);
if (match) {
printf("\nmeasuring half-mass radius: %.7f \t %.7f (should/is)\nand correcting for this factor\n",Rh, Rh3D);
rvir = rvir *Rh/Rh3D;
}
//printf ("\nrvir = %.5f\t rh = %.5f\t rtide = %.5f (pc)\n", rvir, Rh, rtide);
//printf("Edge radius (King units) = %g\t(Nbody units) = %g\n", rking, rking/rvirtemp);
//printf("Core radius (King units) = %g\t(Nbody units) = %g\n\n", 1.0, 1.0/rvirtemp);
//printf("Concentration = %g\n", log10(rking));
} else if (profile == 2) {
double ke = 0;
#ifndef NOOMP
#pragma omp parallel shared(N, star) private(i)
{
#pragma omp for reduction(+: ke) schedule(dynamic)
#endif
for (i=0;i<N;i++) {
ke += M*star[i][0]*(pow(star[i][4],2)+pow(star[i][5],2)+pow(star[i][6],2));
}
#ifndef NOOMP
}
#endif
ke /= 0.5*N;
printf("Dynamical temperature of centre-of-mass particles kT = %lf\n\n",ke);
//make half-mass radius of the system match the desired one
radial_profile(star, N, rvir, M, 0, 0, code, &NNBMAX, &RS0, &Rh2D, &Rh3D, NNBMAX_NBODY6);
printf("\nmeasuring half-mass radius: %.7f \t %.7f (should/is)\nand correcting for this factor\n",Rh, Rh3D);
rvir = rvir *Rh/Rh3D;
}
//Calculate radial density profile, estimate NNBMAX and RS0 (important for Nbody6 only)
radial_profile(star, N, rvir, M, create_radial_profile, create_cumulative_profile, code, &NNBMAX, &RS0, &Rh2D, &Rh3D, NNBMAX_NBODY6);
printf("\nActual half-mass radius of the cluster = (%.4f / %.4f) pc (3D / 2D)\n", Rh3D, Rh2D);
//scale RS0 to nbody units for Nbody6
RS0 /= 1.0*rvir;
/*********************
* Generate Binaries *
*********************/
printf("\n\n-----GENERATE BINARIES----- \n");
if ((!fbin) && (!nbin)) {
printf("\nNo primordial binaries!\n");
} else {
//re-create original array with Nstars (original N) entries
columns = 15;
double **star_temp;
star_temp = (double **)calloc(Nstars,sizeof(double *));
for (j=0;j<Nstars;j++){
star_temp[j] = (double *)calloc(columns,sizeof(double));
if (star_temp[j] == NULL) {
printf("\nMemory allocation failed!\n");
return 0;
}
}
double **mbin_index; //sort mbin by identifier
mbin_index = (double **)calloc(nbin,sizeof(double *));
for (j=0;j<nbin;j++){
mbin_index[j] = (double *)calloc(2,sizeof(double));
if (mbin_index[j] == NULL) {
printf("\nMemory allocation failed!\n");
return 0;
}
}
for (j=0;j<nbin;j++) {
mbin_index[j][0] = mbin[j][15];
mbin_index[j][1] = j;
}
shellsort(mbin_index,nbin,2);
double **star_index;//sort star by identifier
star_index = (double **)calloc(N,sizeof(double *));
for (j=0;j<N;j++){
star_index[j] = (double *)calloc(2,sizeof(double));
if (star_index[j] == NULL) {
printf("\nMemory allocation failed!\n");
return 0;
}
}
for (j=0;j<N;j++) {
star_index[j][0] = star[j][7];
star_index[j][1] = j;
}
shellsort(star_index,N,2);
int p;
for (j=0;j<nbin;j++) {
if (mbin[(int) mbin_index[j][1]][15] == star[(int) star_index[j][1]][7]) {
star_temp[2*j][0] = mbin[(int) mbin_index[j][1]][1]/(1.0*M);//primary mass
star_temp[2*j+1][0] = mbin[(int) mbin_index[j][1]][2]/(1.0*M);//secondary mass
star_temp[2*j][7] = mbin[(int) mbin_index[j][1]][3];//primary m0
star_temp[2*j+1][7] = mbin[(int) mbin_index[j][1]][9];//secondary m0
star_temp[2*j][8] = mbin[(int) mbin_index[j][1]][4];//primary kw
star_temp[2*j+1][8] = mbin[(int) mbin_index[j][1]][10];//secondary kw
star_temp[2*j][9] = mbin[(int) mbin_index[j][1]][5];//primary epoch
star_temp[2*j+1][9] = mbin[(int) mbin_index[j][1]][11];//secondary epoch
star_temp[2*j][10] = mbin[(int) mbin_index[j][1]][6];//primary spin
star_temp[2*j+1][10] = mbin[(int) mbin_index[j][1]][12];//secondary spin
star_temp[2*j][11] = mbin[(int) mbin_index[j][1]][7];//primary r
star_temp[2*j+1][11] = mbin[(int) mbin_index[j][1]][13];//secondary r
star_temp[2*j][12] = mbin[(int) mbin_index[j][1]][8];//primary lum
star_temp[2*j+1][12] = mbin[(int) mbin_index[j][1]][14];//secondary lum
star_temp[2*j][13] = mbin[(int) mbin_index[j][1]][16];//primary epochstar
star_temp[2*j+1][13] = mbin[(int) mbin_index[j][1]][17];//secondary epochstar
star_temp[2*j][14] = mbin[(int) mbin_index[j][1]][18];//primary Zstar
star_temp[2*j+1][14] = mbin[(int) mbin_index[j][1]][19];//secondary Zstar
for (p=1;p<7;p++) {
star_temp[2*j][p] = star[(int) star_index[j][1]][p];
star_temp[2*j+1][p] = star[(int) star_index[j][1]][p];
}
}
}
for (j=nbin;j<N;j++) {
for (p=0;p<columns;p++) {
star_temp[j+nbin][p] = star[(int) star_index[j][1]][p];
}
}
N += nbin;
for (j=0;j<N;j++)
for (p=0;p<columns;p++) star[j][p] = star_temp[j][p]; //copy temporary array back to original
for (j=0;j<Nstars;j++) free (star_temp[j]);
free(star_temp);
printf("\nCreating %i primordial binary systems, fraction: %6.2f percent.\n", nbin, 2.0*nbin/N*100.0);
if (seed) srand48(seed);
get_binaries(nbin, star, M, rvir, pairing, &N, adis, amin, amax, Rh, eigen, BSE, epoch, Z, remnant, OBperiods, msort);
}
//Specify KZ(22) & the sse parameter
#ifdef SSE
if (epoch) sse = 1; //If feeding an evolved stellar population to Nbody6, KZ(12) has to be =2 in order to read-in fort.12
else sse = 0;
#else
sse = 0;
#endif
bin = 4; //KZ(22)
/***********
* Scaling *
***********/
printf("\n\n-----SCALING----- \n");
// Notice the total mass is changed after get_binaries, thus the total/mean mass should be updated
double Mnew = 0;
for(j=0; j<N; j++) Mnew += star[j][0]*M;
mmean = Mnew/N;
printf("\nRe-calculate the total mass after binary generation for scaling: Mnew=%f ",Mnew);
//scale masses, pos & vel to astrophysical units or Nbody units
tscale = sqrt(rvir*rvir*rvir/(G*Mnew));
printf("\nTime scaling: tscale=%f ",tscale);