mirror of
https://codeberg.org/Yael-II/MSc1-Internship-Stellar-Cluster.git
synced 2026-03-15 03:16:26 +01:00
Add files via upload
This commit is contained in:
Yaël M
6
COSMIC/cosmic.sh
Normal file
6
COSMIC/cosmic.sh
Normal file
@@ -0,0 +1,6 @@
|
||||
if [[ "$VIRTUAL_ENV" == "/Users/yael/.venv/amuse" ]]
|
||||
then
|
||||
mpirun -n 1 python source/COSMIC_v3.py
|
||||
else
|
||||
echo "please activate amuse"
|
||||
fi
|
||||
20
COSMIC/input/default.cfg
Normal file
20
COSMIC/input/default.cfg
Normal file
@@ -0,0 +1,20 @@
|
||||
N_stars 10
|
||||
timestep 1
|
||||
output_times 1 2 5 10 20 50 100 200 500 1000 2000 5000
|
||||
R0_king 1
|
||||
W0_king 9
|
||||
metallicity_stellar 0.02
|
||||
M_min_salpeter 0.1
|
||||
M_max_salpeter 125
|
||||
a_salpeter -2.35
|
||||
binary_fraction 0.13
|
||||
mean_period 4.54
|
||||
std_period 2.4
|
||||
X_coefficient_OBA 1.4e-7
|
||||
X_coefficient_GKM 1.4e27
|
||||
out_directory ./output/
|
||||
in_directory ./input/
|
||||
config default.cfg
|
||||
workers_stellar 1
|
||||
workers_gravity 1
|
||||
format_type csv
|
||||
385
COSMIC/old/COSMIC-VIS_v2.py
Normal file
385
COSMIC/old/COSMIC-VIS_v2.py
Normal file
@@ -0,0 +1,385 @@
|
||||
"""
|
||||
* COSMIC-VIS : Cluster Orbital SysteM Integration Code - Visualisation
|
||||
* Version 2 - 2024-02-27
|
||||
@ Yaël Moussouni
|
||||
@ Unistra, P&E, MSc1-MoFP
|
||||
@ Observatory of Strasbourg (Intern)
|
||||
"""
|
||||
import numpy as np
|
||||
import matplotlib.pyplot as plt
|
||||
import matplotlib.animation as animation
|
||||
import os
|
||||
|
||||
# * Parameters
|
||||
if "YII" in plt.style.available: plt.style.use("YII")
|
||||
|
||||
if "YII_light" in plt.style.available: light = "YII_light"
|
||||
else: light = "default"
|
||||
|
||||
# * Variables
|
||||
|
||||
in_directory = "./COSMIC_output/"
|
||||
out_directory = "../Figs/COSMIC_figs/"
|
||||
|
||||
cluster_suffix = "_cluster.csv"
|
||||
stars_suffix = "_stars.csv"
|
||||
|
||||
YES = ["Y", "YES", "1", "OUI"]
|
||||
MARKER = ["o", "s", "D", "v", "^", "<", ">"]
|
||||
|
||||
Tmin = 2000 # K - Temperature truncation
|
||||
Tmax = 10000 # K - Temperature truncation
|
||||
|
||||
# * Functions
|
||||
|
||||
def density_hist(X,Y,M,T,bins,i):
|
||||
x_cm = np.average(X[i], weights=M[i])
|
||||
y_cm = np.average(Y[i], weights=M[i])
|
||||
Radius = np.sqrt((X[i]-x_cm)**2 + (Y[i]-y_cm)**2)
|
||||
Rho = np.zeros(len(bins)-1)
|
||||
for k in range(len(bins)-1):
|
||||
r1 = bins[k]
|
||||
r2 = bins[k+1]
|
||||
w = np.where((Radius > r1) & (Radius < r2))
|
||||
Rho[k] = np.sum(M[i,w])/(4*np.pi*r2**3/3 - 4*np.pi*r1**3/3)
|
||||
return Rho
|
||||
|
||||
# * Listing files for selection
|
||||
filelist = np.sort(os.listdir(in_directory))
|
||||
filelist = [f for f in filelist if f[0] != "."]
|
||||
dates = []
|
||||
for f in filelist:
|
||||
if len(f) == len("YYYY-MM-DD_HH:MM_cluster.csv") or len(f) == len("YYYY-MM-DD_HH:MM_stars.csv"):
|
||||
date = f[0:16]
|
||||
if not date in dates:
|
||||
dates.append(date)
|
||||
|
||||
# * File selection
|
||||
print("\033[36m"+"Available dates:"+"\033[0m")
|
||||
for i in range(len(dates)):
|
||||
print("\033[36m"+"\t{}: ".format(i+1) + "\033[0m" + "{}".format(dates[i].replace("h", ":").replace("_", " ")))
|
||||
j = int(input("\033[32m"+"Select a date number: "+"\033[0m"))-1
|
||||
print("")
|
||||
date_prefix = dates[j]
|
||||
|
||||
# * Data collection
|
||||
cluster = np.loadtxt(in_directory+date_prefix+cluster_suffix, skiprows=1, comments="#", delimiter=",")
|
||||
stars = np.loadtxt(in_directory+date_prefix+stars_suffix, skiprows=1, comments="#", delimiter=",")
|
||||
|
||||
T = cluster[:,1]
|
||||
E = cluster[:,2]
|
||||
DE = cluster[:,3]
|
||||
L = cluster[:,4]
|
||||
DL = cluster[:,5]
|
||||
|
||||
M = np.zeros(np.int32(stars[-1,0:2])+1)
|
||||
X = np.zeros(np.int32(stars[-1,0:2])+1)
|
||||
Y = np.zeros(np.int32(stars[-1,0:2])+1)
|
||||
Z = np.zeros(np.int32(stars[-1,0:2])+1)
|
||||
VX = np.zeros(np.int32(stars[-1,0:2])+1)
|
||||
VY = np.zeros(np.int32(stars[-1,0:2])+1)
|
||||
VZ = np.zeros(np.int32(stars[-1,0:2])+1)
|
||||
Lumi = np.zeros(np.int32(stars[-1,0:2])+1)
|
||||
Radi = np.zeros(np.int32(stars[-1,0:2])+1)
|
||||
Temp = np.zeros(np.int32(stars[-1,0:2])+1)
|
||||
|
||||
for star in stars:
|
||||
i = np.int32(star[0])
|
||||
j = np.int32(star[1])
|
||||
M[i,j] = star[2]
|
||||
X[i,j] = star[3]
|
||||
Y[i,j] = star[4]
|
||||
Z[i,j] = star[5]
|
||||
VX[i,j] = star[6]
|
||||
VY[i,j] = star[7]
|
||||
VZ[i,j] = star[8]
|
||||
Lumi[i,j] = star[9]
|
||||
Radi[i,j] = star[10]
|
||||
Temp[i,j] = star[11]
|
||||
N_iter = i
|
||||
N_part = j
|
||||
|
||||
x_cm = np.array([np.average(X[i], weights=M[i]) for i in range(N_iter)])
|
||||
y_cm = np.array([np.average(Y[i], weights=M[i]) for i in range(N_iter)])
|
||||
z_cm = np.array([np.average(Z[i], weights=M[i]) for i in range(N_iter)])
|
||||
|
||||
lim_min = np.min((X,Y))
|
||||
lim_max = np.max((X,Y))
|
||||
Alpha = np.clip((np.log(Lumi) - np.min(np.log(Lumi)))/(np.max(np.log(Lumi)) - np.min(np.log(Lumi))), 0.1, 1)
|
||||
|
||||
# * Output choice
|
||||
print("\033[36m"+"Choose figures:"+"\033[0m")
|
||||
figure_1 = input("\033[32m"+"\tFigure 1 (energy, angular momentum, time): "+"\033[0m").upper() in YES
|
||||
figure_2 = input("\033[32m"+"\tFigure 2a and 2b (positions, speed): "+"\033[0m").upper() in YES
|
||||
figure_3 = input("\033[32m"+"\tFigure 3 (mass distribution): "+"\033[0m").upper() in YES
|
||||
figure_4 = input("\033[32m"+"\tFigure 4 (density distribution): "+"\033[0m").upper() in YES
|
||||
figure_5 = input("\033[32m"+"\tFigure 5 (HR diagram): "+"\033[0m").upper() in YES
|
||||
print("")
|
||||
|
||||
print("\033[36m"+"General settings:"+"\033[0m")
|
||||
time = np.int32(input("\033[32m"+"\tStatic images drawing instant ({} < int < {}): ".format(0,N_iter)+"\033[0m"))
|
||||
if input("\033[32m"+"\tWindow size restriction (y/n): "+"\033[0m").upper() in YES:
|
||||
lim = np.float32(input("\033[32m"+"\t\tLimit [pc]: "+"\033[0m"))
|
||||
lim_min = -lim/2
|
||||
lim_max = +lim/2
|
||||
print("")
|
||||
|
||||
draw_time = scatter_time = distrib_time = diagram_time = time
|
||||
|
||||
if figure_1:
|
||||
print("\033[36m"+"Figure 1 (energy, angular momentum, time):"+"\033[0m")
|
||||
plot_E = input("\033[32m"+"\tPlot energy vs. time (y/n): "+"\033[0m").upper() in YES
|
||||
plot_L = input("\033[32m"+"\tPlot angular momentum vs. time (y/n): "+"\033[0m").upper() in YES
|
||||
plot_save = input("\033[32m"+"\tSave figure (y/n): "+"\033[0m").upper() in YES
|
||||
print("")
|
||||
else: plot_E = plot_L = plot_save = False
|
||||
|
||||
if figure_2:
|
||||
print("\033[36m"+"Figure 2a and 2b (positions, speed):"+"\033[0m")
|
||||
scatter_2D = input("\033[32m"+"\tScatter positions in 2D (y/n): "+"\033[0m").upper() in YES
|
||||
scatter_3D = input("\033[32m"+"\tScatter positions in 3D (y/n): "+"\033[0m").upper() in YES
|
||||
scatter_speed = input("\033[32m"+"\tShow speed vectors (y/n): "+"\033[0m").upper() in YES
|
||||
scatter_save = input("\033[32m"+"\tSave figure (y/n): "+"\033[0m").upper() in YES
|
||||
scatter_animate = input("\033[32m"+"\tAnimate over time (y/n): "+"\033[0m").upper() in YES
|
||||
print("")
|
||||
else: scatter_2D = scatter_3D = scatter_speed = scatter_save = scatter_animate = False
|
||||
|
||||
if figure_3:
|
||||
print("\033[36m"+"Figure 3 (mass distribution):"+"\033[0m")
|
||||
distrib_mass = input("\033[32m"+"\tShow mass distribution (y/n): "+"\033[0m").upper() in YES
|
||||
distrib_bins = np.int32(input("\033[32m"+"\tNumber of bins (int): "+"\033[0m"))
|
||||
distrib_save = input("\033[32m"+"\tSave figure (y/n): "+"\033[0m").upper() in YES
|
||||
print("")
|
||||
else: distrib_mass = distrib_bins = distrib_save = False
|
||||
|
||||
if figure_4:
|
||||
print("\033[36m"+"Figure 4 (density distribution):"+"\033[0m")
|
||||
draw_density = input("\033[32m"+"\tShow density distribution (y/n): "+"\033[0m").upper() in YES
|
||||
draw_bins = np.float32(input("\033[32m"+"\tWidth of bins [pc]: "+"\033[0m"))
|
||||
draw_max = np.float32(input("\033[32m"+"\tMaximum distance [pc]: "+"\033[0m"))
|
||||
draw_save = input("\033[32m"+"\tSave figure (y/n): "+"\033[0m").upper() in YES
|
||||
draw_animate = input("\033[32m"+"\tAnimate over time (y/n): "+"\033[0m").upper() in YES
|
||||
print("")
|
||||
else: draw_density = draw_bins = draw_max = draw_save = draw_animate = False
|
||||
|
||||
if figure_5:
|
||||
print("\033[36m"+"Figure 5 (HR diagram):"+"\033[0m")
|
||||
diagram_HT = input("\033[32m"+"\tDraw HR diagram (y/n): "+"\033[0m").upper() in YES
|
||||
diagram_save = input("\033[32m"+"\tSave figure (y/n): "+"\033[0m").upper() in YES
|
||||
diagram_animate = input("\033[32m"+"\tAnimate over time (y/n): "+"\033[0m").upper() in YES
|
||||
else : diagram_HT = diagram_save = diagram_animate = False
|
||||
|
||||
# * Plotting
|
||||
if plot_E or plot_L:
|
||||
fig1, axs1 = plt.subplots(2, sharex=True)
|
||||
if plot_E and not plot_L: # Just the energy
|
||||
axs1[1].set_xlabel("$t\\ [\\mathrm{{Myr}}]$")
|
||||
axs1[0].set_ylabel("$E\\ [\\mathrm{{pc^2\\ M_\\odot\\ Myr^{{-2}}}}]$")
|
||||
axs1[1].set_ylabel("$\\Delta E/E_0$")
|
||||
axs1[0].plot(T, E, color="C3")
|
||||
axs1[1].plot(T, DE, color="C3")
|
||||
elif plot_L and not plot_E: # Just the angular momentum
|
||||
axs1[1].set_xlabel("$t\\ [\\mathrm{{Myr}}]$")
|
||||
axs1[0].set_ylabel("$L\\ [\\mathrm{{pc^2\\ M_\\odot\\ Myr^{{-1}}}}]$")
|
||||
axs1[1].set_ylabel("$\\Delta L/L_0$")
|
||||
axs1[0].plot(T, L, color="C4")
|
||||
axs1[1].plot(T, DL, color="C4")
|
||||
elif plot_L and plot_E: # ...both
|
||||
xas1 = [axs1[i].twinx() for i in range(len(axs1))]
|
||||
axs1[1].set_xlabel("$t\\ [\\mathrm{{Myr}}]$")
|
||||
axs1[0].set_ylabel("$E\\ [\\mathrm{{pc^2\\ M_\\odot\\ Myr^{{-2}}}}]$")
|
||||
axs1[1].set_ylabel("$\\Delta E/E_0$")
|
||||
xas1[0].set_ylabel("$L\\ [\\mathrm{{pc^2\\ M_\\odot\\ Myr^{{-1}}}}]$")
|
||||
xas1[1].set_ylabel("$\\Delta L/L_0$")
|
||||
axs1[0].plot(T, E, color="C3")
|
||||
axs1[1].plot(T, DE, color="C3")
|
||||
xas1[0].plot(T, L, color="C4")
|
||||
xas1[1].plot(T, DL, color="C4")
|
||||
axs1[0].tick_params(axis='y', which="both", colors='C3')
|
||||
axs1[0].yaxis.label.set_color('C3')
|
||||
xas1[0].tick_params(axis='y', which="both", colors='C4')
|
||||
xas1[0].yaxis.label.set_color('C4')
|
||||
axs1[1].tick_params(axis='y', which="both", colors='C3')
|
||||
axs1[1].yaxis.label.set_color('C3')
|
||||
xas1[1].tick_params(axis='y', which="both", colors='C4')
|
||||
xas1[1].yaxis.label.set_color('C4')
|
||||
if plot_save:
|
||||
fig1.tight_layout()
|
||||
fig1.savefig(out_directory+date_prefix+"_figure_1")
|
||||
print("\033[94m"+"Info: Figure saved as " + "\033[0m" + date_prefix+"_figure_1")
|
||||
|
||||
if scatter_2D or scatter_3D:
|
||||
if scatter_2D:
|
||||
fig2a, ax2a = plt.subplots(1)
|
||||
# ax2a.set_facecolor('k')
|
||||
i = scatter_time
|
||||
ax2a.set_title("$t =$ {:.2f} Myr".format(T[i]))
|
||||
if scatter_speed:
|
||||
qvr2a = ax2a.quiver(X[i]-x_cm[i],Y[i]-y_cm[i],VX[i],VY[i], alpha=0.1, headwidth=2, headlength=2, headaxislength=2, color="k")
|
||||
ax2a.quiverkey(qvr2a, 0.95, 0.05, 1, "Velocity scale: $1\mathrm{{~km\\cdot s^{{-1}}}}$", labelpos='W', coordinates='figure', color="k", alpha=1)
|
||||
sct2a = ax2a.scatter(X[i]-x_cm[i],Y[i]-y_cm[i],s=np.clip(Radi[i]**2,0.5,30), c=Temp[i], alpha=Alpha[i], cmap="RdYlBu", vmin=Tmin, vmax=Tmax)
|
||||
ax2a.set_xlabel("$x$ [pc]")
|
||||
ax2a.set_ylabel("$y$ [pc]")
|
||||
ax2a.set_xlim(lim_min, lim_max)
|
||||
ax2a.set_ylim(lim_min, lim_max)
|
||||
ax2a.set_aspect("equal")
|
||||
fig2a.colorbar(sct2a, label="Stellar effective temperature $T$ [K]", extend='both')
|
||||
fig2a.tight_layout()
|
||||
if scatter_save:
|
||||
fig2a.savefig(out_directory+date_prefix+"_figure_2a")
|
||||
print("\033[94m"+"Info: Figure saved as " + "\033[0m" + date_prefix+"_figure_2a")
|
||||
if scatter_3D:
|
||||
fig2b, ax2b = plt.subplots(1, subplot_kw={"projection": "3d"})
|
||||
# ax2b.set_facecolor('k')
|
||||
i = scatter_time
|
||||
ax2b.set_title("$t =$ {:.2f} Myr".format(T[i]))
|
||||
if scatter_speed:
|
||||
qvr2b = ax2b.quiver(X[i]-x_cm[i],Y[i]-y_cm[i],Z[i]-z_cm[i],VX[i],VY[i],VZ[i], alpha=0.1, color="k")
|
||||
# ax2b.quiverkey(qvr2b, 0.95, 0.05, 2, "Velocity scale: $2\mathrm{{~km\\cdot s^{{-1}}}}$", labelpos='W', coordinates='figure')
|
||||
sct2b = ax2b.scatter(X[i]-x_cm[i],Y[i]-y_cm[i],Z[i]-z_cm[i],s=np.clip(Radi[i]**2,0.5,30), c=Temp[i], alpha=Alpha[i], cmap="RdYlBu", vmin=Tmin, vmax=Tmax)
|
||||
ax2b.set_xlabel("$x$ [pc]")
|
||||
ax2b.set_ylabel("$y$ [pc]")
|
||||
ax2b.set_zlabel("$z$ [pc]")
|
||||
ax2b.set_xlim(lim_min, lim_max)
|
||||
ax2b.set_ylim(lim_min, lim_max)
|
||||
ax2b.set_zlim(lim_min, lim_max)
|
||||
ax2b.set_aspect("equal")
|
||||
fig2b.colorbar(sct2b, label="Stellar effective temperature $T$ [K]", location="left", extend='both')
|
||||
fig2b.tight_layout()
|
||||
if scatter_save:
|
||||
fig2b.savefig(out_directory+date_prefix+"_figure_2b")
|
||||
print("\033[94m"+"Info: Figure saved as " + "\033[0m" + date_prefix+"_figure_2b")
|
||||
|
||||
if distrib_mass:
|
||||
fig3, ax3 = plt.subplots(1)
|
||||
i = distrib_time
|
||||
ax3.set_title("$t =$ {:.2f} Myr".format(T[i]))
|
||||
nbins = distrib_bins
|
||||
hist, lbin = np.histogram(M[i], nbins)
|
||||
cbins = 0.5*(lbin[1:]+ lbin[: -1])
|
||||
ax3.scatter(cbins, hist, s=5)
|
||||
ax3.set_xscale ("log")
|
||||
ax3.set_yscale ("log")
|
||||
ax3.set_xlabel("Masses $M\\ [\\mathrm{{M_\\odot}}]$")
|
||||
ax3.set_ylabel("Star distribution")
|
||||
if distrib_save:
|
||||
fig3.savefig(out_directory+date_prefix+"_figure_3")
|
||||
print("\033[94m"+"Info: Figure saved as " + "\033[0m" + date_prefix+"_figure_3")
|
||||
|
||||
if draw_density:
|
||||
fig4, ax4 = plt.subplots(1)
|
||||
i = draw_time
|
||||
bin_width = draw_bins
|
||||
bin_max = draw_max
|
||||
bins = np.arange(0,bin_max,bin_width)
|
||||
Rho = density_hist(X,Y,M,T,bins,i)
|
||||
cbins = 0.5*(bins[1:]+ bins[: -1])
|
||||
ax4.set_title("$t =$ {:.2f} Myr".format(T[i]))
|
||||
ax4.set_xscale ("log")
|
||||
ax4.set_yscale ("log")
|
||||
ax4.set_xlabel("Distance from center $r$ [pc]")
|
||||
ax4.set_ylabel("Stellar masses density $\\rho\\ [\\mathrm{{M_\\odot\\ pc^{{-3}}}}]$")
|
||||
ax4.scatter(cbins, Rho, s=5)
|
||||
fig4.tight_layout()
|
||||
if draw_save:
|
||||
fig4.savefig(out_directory+date_prefix+"_figure_4")
|
||||
print("\033[94m"+"Info: Figure saved as " + "\033[0m" + date_prefix+"_figure_4")
|
||||
|
||||
if diagram_HT:
|
||||
fig5, ax5 = plt.subplots(1)
|
||||
ax5.invert_xaxis()
|
||||
i = diagram_time
|
||||
ax5.set_title("$t =$ {:.2f} Myr".format(T[i]))
|
||||
ax5.set_xlabel("Temperature $T$ [K]")
|
||||
ax5.set_ylabel("Luminosity $L\\ [\\mathrm{{L_\\odot}}]$")
|
||||
ax5.set_xscale ("log")
|
||||
ax5.set_yscale ("log")
|
||||
ax5.scatter(Temp[i], Lumi[i], s=5, alpha=Alpha[i], c=Temp[i], cmap="RdYlBu", vmin=Tmin, vmax=Tmax)
|
||||
fig5.tight_layout()
|
||||
if diagram_save:
|
||||
fig5.savefig(out_directory+date_prefix+"_figure_5")
|
||||
print("\033[94m"+"Info: Figure saved as " + "\033[0m" + date_prefix+"_figure_5")
|
||||
|
||||
if scatter_animate:
|
||||
figA2a,axA2a = plt.subplots(1)
|
||||
# ax2a.set_facecolor('k')
|
||||
axA2a.set_title("$t =$ {:.2f} Myr".format(T[0]))
|
||||
if scatter_speed:
|
||||
qvr = axA2a.quiver(X[0]-x_cm[0],Y[0]-y_cm[0],VX[0],VY[0], alpha=0.5, headwidth=2, headlength=2, headaxislength=2, color="k")
|
||||
axA2a.quiverkey(qvr, 0.95, 0.05, 1, "Velocity scale: $1\mathrm{{~km\\cdot s^{{-1}}}}$", labelpos='W', coordinates='figure', color="k", alpha=1)
|
||||
sctA2a = axA2a.scatter(X[0]-x_cm[0],Y[0]-y_cm[0],s=np.clip(Radi[0]**2,0.5,30), c=Temp[0], alpha=Alpha[0], cmap="RdYlBu", vmin=Tmin, vmax=Tmax)
|
||||
figA2a.colorbar(sctA2a, label="Stellar effective temperature $T$ [K]", extend='both')
|
||||
axA2a.set_xlabel("$x$ [pc]")
|
||||
axA2a.set_ylabel("$y$ [pc]")
|
||||
axA2a.set_aspect("equal")
|
||||
axA2a.set_xlim(lim_min, lim_max)
|
||||
axA2a.set_ylim(lim_min, lim_max)
|
||||
figA2a.tight_layout()
|
||||
def anim2a(i):
|
||||
if scatter_speed:
|
||||
qvr.set_offsets(np.array([X[i]-x_cm[i],Y[i]-y_cm[i]]).T)
|
||||
qvr.set_UVC(VX[i],VY[i])
|
||||
axA2a.set_title("$t =$ {:.2f} Myr".format(T[i]))
|
||||
sctA2a.set_offsets(np.array([X[i]-x_cm[i],Y[i]-y_cm[i]]).T)
|
||||
sctA2a.set_array(Temp[i])
|
||||
sctA2a.set_sizes(np.clip(Radi[i]**2,0.5,30))
|
||||
sctA2a.set_alpha(Alpha[i])
|
||||
return sctA2a,
|
||||
|
||||
ani2a = animation.FuncAnimation(fig=figA2a, func=anim2a, frames=N_iter, interval=100)
|
||||
if scatter_save:
|
||||
ani2a.save(out_directory+date_prefix+"_animation_2a.png", dpi=300, fps=10)
|
||||
ani2a.save(out_directory+date_prefix+"_animation_2a.pdf", dpi=300, fps=10)
|
||||
print("\033[94m"+"Info: Animation saved as " + "\033[0m" + date_prefix+"_animation_2a")
|
||||
|
||||
|
||||
if draw_animate:
|
||||
figA4, axA4 = plt.subplots(1)
|
||||
bin_width = draw_bins
|
||||
bin_max = draw_max
|
||||
bins = np.arange(0,bin_max,bin_width)
|
||||
cbins = 0.5*(bins[1:]+ bins[: -1])
|
||||
Rho = np.array([density_hist(X,Y,M,T,bins,k) for k in range(N_iter)])
|
||||
axA4.set_title("$t =$ {:.2f} Myr".format(T[0]))
|
||||
sctA4 = axA4.scatter(cbins, Rho[0], s=5)
|
||||
axA4.set_xscale ("log")
|
||||
axA4.set_yscale ("log")
|
||||
axA4.set_ylim(top=np.max(Rho))
|
||||
axA4.set_xlabel("Distance from center $r$ [pc]")
|
||||
axA4.set_ylabel("Stellar masses density $\\rho\\ [\\mathrm{{M_\\odot\\ pc^{{-3}}}}]$")
|
||||
figA4.tight_layout()
|
||||
def anim4(i):
|
||||
axA4.set_title("$t =$ {:.2f} Myr".format(T[i]))
|
||||
sctA4.set_offsets(np.array([cbins, Rho[i]]).T)
|
||||
return sctA4
|
||||
ani4 = animation.FuncAnimation(fig=figA4, func=anim4, frames=N_iter, interval=100)
|
||||
if scatter_save:
|
||||
ani4.save(out_directory+date_prefix+"_animation_4.png", dpi=300, fps=10)
|
||||
ani4.save(out_directory+date_prefix+"_animation_4.pdf", dpi=300, fps=10)
|
||||
print("\033[94m"+"Info: Animation saved as " + "\033[0m" + date_prefix+"_animation_4")
|
||||
|
||||
if diagram_animate:
|
||||
figA5, axA5 = plt.subplots(1)
|
||||
axA5.invert_xaxis()
|
||||
axA5.set_title("$t =$ {:.2f} Myr".format(T[0]))
|
||||
axA5.set_xlabel("Temperature $T$ [K]")
|
||||
axA5.set_ylabel("Luminosity $L\\ [\\mathrm{{L_\\odot}}]$")
|
||||
axA5.set_xscale ("log")
|
||||
axA5.set_yscale ("log")
|
||||
axA5.set_xlim(np.max(Temp), np.min(Temp))
|
||||
axA5.set_ylim(np.min(Lumi), np.max(Lumi))
|
||||
sctA5 = axA5.scatter(Temp[0], Lumi[0], s=5, alpha=Alpha[0], c=Temp[0], cmap="RdYlBu", vmin=Tmin, vmax=Tmax)
|
||||
fig5.tight_layout()
|
||||
def anim5(i):
|
||||
axA5.set_title("$t =$ {:.2f} Myr".format(T[i]))
|
||||
sctA5.set_offsets(np.array([Temp[i], Lumi[i]]).T)
|
||||
sctA5.set_array(Temp[i])
|
||||
ani5 = animation.FuncAnimation(fig=figA5, func=anim5, frames=N_iter, interval=100)
|
||||
if diagram_save:
|
||||
ani5.save(out_directory+date_prefix+"_animation_5.png", dpi=300, fps=10)
|
||||
ani5.save(out_directory+date_prefix+"_animation_5.pdf", dpi=300, fps=10)
|
||||
print("\033[94m"+"Info: Animation saved as " + "\033[0m" + date_prefix+"_animation_5")
|
||||
|
||||
# * SHOW !
|
||||
plt.show(block=False)
|
||||
input("(press enter to quit)")
|
||||
164
COSMIC/old/COSMIC_v2.py
Normal file
164
COSMIC/old/COSMIC_v2.py
Normal file
@@ -0,0 +1,164 @@
|
||||
"""
|
||||
* COSMIC : Cluster Orbital SysteM Integration Code
|
||||
* Version 2 - 2024-02-27
|
||||
@ Yaël Moussouni
|
||||
@ Unistra, P&E, MSc1-MoFP
|
||||
@ Observatory of Strasbourg (Intern)
|
||||
"""
|
||||
import numpy as np
|
||||
import amuse.units.units as u
|
||||
import datetime
|
||||
|
||||
|
||||
from amuse.units import nbody_system
|
||||
from amuse.ic.kingmodel import new_king_model
|
||||
from amuse.ic.salpeter import new_salpeter_mass_distribution
|
||||
from amuse.datamodel.particles import Channels
|
||||
from amuse.community.ph4.interface import Ph4
|
||||
from amuse.community.seba.interface import SeBa
|
||||
from amuse.couple.bridge import Bridge
|
||||
|
||||
|
||||
# * Parameters
|
||||
N_part = 10 # Number of particle
|
||||
N_iter = 30 # Number of iteration
|
||||
dt = 1|u.Myr # Time increment
|
||||
|
||||
R0 = 1|u.parsec # Radius of the system
|
||||
W0 = 9 # King parameter
|
||||
z = 0.02 # Metallicity
|
||||
|
||||
# * Variables
|
||||
date = datetime.datetime.now()
|
||||
date = "{:04d}-{:02d}-{:02d}_{:02d}h{:02d}".format(date.year, date.month, date.day, date.hour, date.minute)
|
||||
|
||||
directory = "./output/"
|
||||
filename_cluster = "{}_cluster.csv".format(date)
|
||||
filename_stars = "{}_stars.csv".format(date)
|
||||
|
||||
# * Function
|
||||
def get_total_momentum(M, X, V):
|
||||
"""
|
||||
Compute the total momentum of particles with mass M, positions X and velocities V.
|
||||
"""
|
||||
l = 0
|
||||
for j in range(len(X)):
|
||||
m = M[j].value_in(u.MSun)
|
||||
x = X[j].value_in(u.pc)
|
||||
v = V[j].value_in(u.pc/u.Myr)
|
||||
l += m*np.cross(x,v)
|
||||
return np.sqrt(np.sum(l**2))|(u.pc**2 * u.MSun / u.Myr)
|
||||
|
||||
# * Initialization
|
||||
def create_cluster(N:int, R=1|u.pc, W=9):
|
||||
"""
|
||||
Create cluster of N stars of radius R (default: 1 pc) following King model of parameter W (default: 9).
|
||||
"""
|
||||
print("\033[94m"+"Info: Simulation with "+"\033[0m"+"{}".format(N)+"\033[94m"+" stars"+"\033[0m")
|
||||
M_stars = new_salpeter_mass_distribution(N)
|
||||
converter = nbody_system.nbody_to_si(M_stars.sum(), R)
|
||||
stars = new_king_model(N, W, converter)
|
||||
stars.mass = M_stars
|
||||
stars.zams_mass = M_stars
|
||||
return stars, converter
|
||||
|
||||
# * Evolution
|
||||
def stellar_gravity_evolution(stars, converter, t_max=16|u.Myr, dt=1|u.Myr, out_dt=1|u.Myr):
|
||||
"""
|
||||
Evolve a model with both gravity and stellar evolution. dt is the simulation time step, while out_dt is the delay between printing in file.
|
||||
"""
|
||||
print("\033[94m"+"Info: Simulation duration of "+"\033[0m"+"{:.2f} Myr".format(t_max.value_in(u.Myr)))
|
||||
init_files()
|
||||
|
||||
gravity = Ph4(converter) # gravity model
|
||||
stellar = SeBa() # stellar model
|
||||
bridge = Bridge() # bridge between models
|
||||
|
||||
# TODO gravity.initialize_code()
|
||||
|
||||
gravity.particles.add_particles(stars)
|
||||
stellar.particles.add_particles(stars)
|
||||
|
||||
stellar.set_metallicity(z)
|
||||
stellar.commit_particles()
|
||||
stellar.update_particles(stars) # TODO pourquoi ?
|
||||
|
||||
bridge.add_system(gravity)
|
||||
bridge.add_system(stellar)
|
||||
|
||||
bridge.synchronize_model()
|
||||
|
||||
bridge.channels.add_channel(stellar.particles.new_channel_to(gravity.particles, attributes=["mass", "radius"]))
|
||||
# Sync the mass and radius between the two models
|
||||
|
||||
out_channel = Channels()
|
||||
out_channel.add_channel(stellar.particles.new_channel_to(stars))
|
||||
out_channel.add_channel(gravity.particles.new_channel_to(stars))
|
||||
|
||||
bridge.timestep = dt # TODO timestep dynamique
|
||||
print(gravity.get_initial_timestep_median()) # TODO ????
|
||||
i = 0
|
||||
t = 0 | u.Myr
|
||||
E0 = gravity.get_total_energy()
|
||||
L0 = get_total_momentum(stars.mass, stars.position, stars.velocity)
|
||||
while t <= t_max:
|
||||
print("\033[36m"+"t: "+"\033[0m"+"{:02.2f} Myr/{:02.2f} Myr".format(t.value_in(u.Myr),t_max.value_in(u.Myr)))
|
||||
bridge.evolve_model(t)
|
||||
out_channel.copy()
|
||||
E = gravity.get_total_energy()
|
||||
L = get_total_momentum(stars.mass, stars.position, stars.velocity)
|
||||
write_files(stars, i, t, E, E0, L, L0)
|
||||
i += 1
|
||||
t += out_dt
|
||||
|
||||
print("\033[36m"+"t: "+"\033[0m"+"{:02.2f} Myr/{:02.2f} Myr".format(t_max.value_in(u.Myr),t_max.value_in(u.Myr)))
|
||||
print("\033[36m"+"Simulation completed"+"\033[0m")
|
||||
return 0
|
||||
|
||||
# * Files initialization and write
|
||||
def init_files():
|
||||
file = open(directory+filename_cluster, "w")
|
||||
file.write("#i (time), t [Myr], E [pc2 MSun Myr-2], (E-E0)/E0, L [pc2 MSun Myr-1], (L-L0)/L0\n")
|
||||
file.close()
|
||||
|
||||
file = open(directory+filename_stars, "w")
|
||||
file.write("#i (time), j (star), m [MSun], x [pc], y [pc], z [pc], vx [km s-1], vy [km s-1], vz [km s-1], L [LSun], R [RSun], T [K]\n")
|
||||
file.close()
|
||||
|
||||
print("\033[94m"+"Info: Created two output files with date " + "\033[0m" + date.replace("h", ":").replace("_", " "))
|
||||
return 0
|
||||
|
||||
def write_files(stars, i, t, E, E0, L, L0):
|
||||
file = open(directory+filename_cluster, "a")
|
||||
file.write("{:d}, ".format(i))
|
||||
file.write("{:+e}, ".format(t.value_in(u.Myr)))
|
||||
file.write("{:+e}, ".format(E.value_in(u.pc**2 * u.MSun * u.Myr**-2)))
|
||||
file.write("{:+e}, ".format((E-E0)/E0))
|
||||
file.write("{:+e}, ".format(L.value_in(u.pc**2 * u.MSun * u.Myr**-1)))
|
||||
file.write("{:+e}\n".format((L-L0)/L0))
|
||||
file.close()
|
||||
|
||||
file = open(directory+filename_stars, "a")
|
||||
for j in range(N_part):
|
||||
file.write("{:d}, ".format(i))
|
||||
file.write("{:d}, ".format(j))
|
||||
file.write("{:+e}, ".format(stars.mass[j].value_in(u.MSun)))
|
||||
file.write("{:+e}, ".format(stars.position[j,0].value_in(u.pc)))
|
||||
file.write("{:+e}, ".format(stars.position[j,1].value_in(u.pc)))
|
||||
file.write("{:+e}, ".format(stars.position[j,2].value_in(u.pc)))
|
||||
file.write("{:+e}, ".format(stars.velocity[j,0].value_in(u.km * u.s**-1)))
|
||||
file.write("{:+e}, ".format(stars.velocity[j,1].value_in(u.km * u.s**-1)))
|
||||
file.write("{:+e}, ".format(stars.velocity[j,2].value_in(u.km * u.s**-1)))
|
||||
file.write("{:+e}, ".format(stars.luminosity[j].value_in(u.LSun)))
|
||||
file.write("{:+e}, ".format(stars.radius[j].value_in(u.RSun)))
|
||||
file.write("{:+e}\n".format(stars.temperature[j].value_in(u.K)))
|
||||
file.close()
|
||||
return 0
|
||||
|
||||
# * Main
|
||||
cluster, nbody_converter = create_cluster(N_part, R0, W0)
|
||||
stellar_gravity_evolution(cluster, nbody_converter, N_iter*dt, dt, dt)
|
||||
|
||||
|
||||
|
||||
|
||||
28
COSMIC/source/COSMIC_v3.py
Normal file
28
COSMIC/source/COSMIC_v3.py
Normal file
@@ -0,0 +1,28 @@
|
||||
"""
|
||||
* COSMIC : Cluster Orbital SysteM Integration Code
|
||||
* Version 3
|
||||
@ Yaël Moussouni
|
||||
@ Unistra, P&E, MSc1-MoFP
|
||||
@ Observatory of Strasbourg (Intern)
|
||||
"""
|
||||
|
||||
import numpy as np
|
||||
import amuse.units.units as u
|
||||
# import matplotlib.pyplot as plt
|
||||
import COSMIC_v3_config as config
|
||||
import COSMIC_v3_init as init
|
||||
import COSMIC_v3_evolve as evolve
|
||||
# import COSMIC_v3_output as output
|
||||
# import COSMIC_v3_emission as emission
|
||||
|
||||
params, params_list = config.default()
|
||||
params = config.from_cfg_file(params)
|
||||
stars, binaries, converter = init.king_salpeter_binaries(params)
|
||||
# stars, converter = init.king_salpeter(params)
|
||||
channels = init.create_channels()
|
||||
codes = init.gravity_stellar_bridge(converter, params)
|
||||
codes = init.add_stars(codes, stars)
|
||||
codes, channels = init.add_binaries(codes, stars, binaries, channels)
|
||||
codes, channels = init.commit(codes, stars, channels, params)
|
||||
codes, stars, channels = evolve.stellar_gravity_binaries(codes, stars, binaries, channels, params, save_stars = True, save_binaries = True, compute_X_emission = True)
|
||||
# evolve.stellar_gravity(codes, stars, channels, params, save_stars = True)
|
||||
96
COSMIC/source/COSMIC_v3_config.py
Normal file
96
COSMIC/source/COSMIC_v3_config.py
Normal file
@@ -0,0 +1,96 @@
|
||||
"""
|
||||
* COSMIC - CONFIG
|
||||
* Version 3
|
||||
@ Yaël Moussouni
|
||||
@ Unistra, P&E, MSc1-MoFP
|
||||
@ Observatory of Strasbourg (Intern)
|
||||
"""
|
||||
|
||||
import numpy as np
|
||||
import amuse.units.units as u
|
||||
import datetime
|
||||
|
||||
def params_dic():
|
||||
params_list = ["N_stars", "timestep", "output_times", "R0_king", "W0_king", "metallicity_stellar", "M_min_salpeter", "M_max_salpeter", "a_salpeter", "binary_fraction", "mean_period", "std_period", "X_coefficient_OBA", "X_coefficient_GKM", "out_directory", "in_directory", "config", "filename", "workers_stellar", "workers_gravity", "format_type"]
|
||||
params = {i:0 for i in params_list}
|
||||
return params, params_list
|
||||
|
||||
def verbatim(params):
|
||||
print("\033[94m"+"Info: Simulation time of "+"\033[0m"+"{:.2f} Myr".format(np.max(params["output_times"].value_in(u.Myr))))
|
||||
print("\033[94m"+"Info: Simulation of "+"\033[0m"+"{:d} stars".format(params["N_stars"]))
|
||||
print("\033[94m"+"Info: Simulation will be saved with the prefix "+"\033[0m"+"{}".format(params["filename"]))
|
||||
print("\033[94m"+"Info: Gravity: "+"\033[0m"+"{:d} workers".format(params["workers_gravity"])+"\033[94m"+", Stellar: "+"\033[0m"+"{:d} workers".format(params["workers_stellar"]))
|
||||
return 0
|
||||
|
||||
def default():
|
||||
params, params_list = params_dic()
|
||||
|
||||
date = datetime.datetime.now()
|
||||
date = "{:04d}-{:02d}-{:02d}_{:02d}h{:02d}".format(date.year, date.month, date.day, date.hour, date.minute)
|
||||
|
||||
params["N_stars"] = np.int32(10) # Number of particle
|
||||
params["timestep"] = np.float32(1)|u.Myr # Time increment
|
||||
params["output_times"] = np.float32([1,2,5,10,20,50,100,200,500,1000,2000,5000])|u.Myr # Output intants
|
||||
params["R0_king"] = np.float32(1)|u.pc # Cluster virial radius
|
||||
params["W0_king"] = np.float32(9) # Cluster King's parameter
|
||||
params["metallicity_stellar"] = np.float32(0.02) # Metallicity
|
||||
params["M_min_salpeter"] = np.float32(0.1)|u.MSun # Minimum mass for Salpeter's law
|
||||
params["M_max_salpeter"] = np.float32(125)|u.MSun # Maximum mass for Salpeter's law
|
||||
params["a_salpeter"] = np.float32(-2.35) # Salpeter's law coefficient
|
||||
params["binary_fraction"] = np.float32(0.13) # Fraction of binary stars
|
||||
params["mean_period"] = np.float32(4.54) # Mean orbital period of binary systems (log10(T/days))
|
||||
params["std_period"] = np.float32(2.4) # Orbital period deviation of binary systems
|
||||
params["X_coefficient_OBA"] = np.float32(1.4e-7) # X-ray luminosity coefficient for O, B and A type stars
|
||||
params["X_coefficient_GKM"] = np.float32(1.4e27) # X-ray luminosity coefficient for G, K and M type stars
|
||||
params["out_directory"] = "./output/"
|
||||
params["in_directory"] = "./input/"
|
||||
params["config"] = "default.cfg"
|
||||
params["filename"] = "COSMIC_{}".format(date)
|
||||
params["workers_stellar"] = np.int32(1)
|
||||
params["workers_gravity"] = np.int32(1)
|
||||
params["format_type"] = "csv"
|
||||
return params, params_list
|
||||
|
||||
def change_params(params, cfg_param, cfg_values):
|
||||
if cfg_param == "":
|
||||
return params
|
||||
elif cfg_param == "N_stars": params["N_stars"] = np.int32(cfg_values[0])
|
||||
elif cfg_param == "timestep": params["timestep"] = np.float32(cfg_values[0])|u.Myr
|
||||
elif cfg_param == "output_times": params["output_times"] = np.float32(cfg_values)|u.Myr
|
||||
elif cfg_param == "R0_king": params["R0_king"] = np.float32(cfg_values[0])|u.pc
|
||||
elif cfg_param == "W0_king": params["W0_king"] = np.float32(cfg_values[0])
|
||||
elif cfg_param == "metallicity_stellar": params["metallicity_stellar"] = np.float32(cfg_values[0])
|
||||
elif cfg_param == "M_min_salpeter": params["M_min_salpeter"] = np.float32(cfg_values[0])|u.MSun
|
||||
elif cfg_param == "M_max_salpeter": params["M_max_salpeter"] = np.float32(cfg_values[0])|u.MSun
|
||||
elif cfg_param == "a_salpeter": params["a_salpeter"] = np.float32(cfg_values[0])
|
||||
elif cfg_param == "binary_fraction": params["binary_fraction"] = np.float32(cfg_values[0])
|
||||
elif cfg_param == "mean_period": params["mean_period"] = np.float32(cfg_values[0])
|
||||
elif cfg_param == "std_period": params["std_period"] = np.float32(cfg_values[0])
|
||||
elif cfg_param == "X_coefficient_OBA": params["X_coefficient_OBA"] = np.float32(cfg_values[0])
|
||||
elif cfg_param == "X_coefficient_GKM": params["X_coefficient_GKM"] = np.float32(cfg_values[0])
|
||||
elif cfg_param == "out_directory": params["out_directory"] = cfg_values[0].replace("\n", "")
|
||||
elif cfg_param == "in_directory": params["in_directory"] = cfg_values[0].replace("\n", "")
|
||||
elif cfg_param == "config": params["config"] = cfg_values[0].replace("\n", "")
|
||||
elif cfg_param == "filename": params["filename"] = cfg_values[0].replace("\n", "")
|
||||
elif cfg_param == "workers_stellar": params["workers_stellar"] = np.int32(cfg_values[0])
|
||||
elif cfg_param == "workers_gravity": params["workers_gravity"] = np.int32(cfg_values[0])
|
||||
elif cfg_param == "format_type": params["format_type"] = cfg_values[0].replace("\n", "")
|
||||
else:
|
||||
print("\033[93m"+"Warning: cannot understand the parameter in config: "+"\033[0m" + cfg_param)
|
||||
return params
|
||||
|
||||
|
||||
def from_cfg_file(params):
|
||||
cfg_path = params["in_directory"] + params["config"]
|
||||
with open(cfg_path, "r") as cfg_file:
|
||||
for cfg_line in cfg_file.readlines():
|
||||
cfg_split = cfg_line.split(" ")
|
||||
if len(cfg_split) == 1:
|
||||
print("\033[93m"+"Warning: cannot understand the line in config: "+"\033[0m" + cfg_line)
|
||||
continue
|
||||
cfg_param = cfg_split[0]
|
||||
cfg_values = cfg_split[1:]
|
||||
params = change_params(params, cfg_param, cfg_values)
|
||||
verbatim(params)
|
||||
return params
|
||||
|
||||
27
COSMIC/source/COSMIC_v3_emission.py
Normal file
27
COSMIC/source/COSMIC_v3_emission.py
Normal file
@@ -0,0 +1,27 @@
|
||||
"""
|
||||
* COSMIC - EMISSION
|
||||
* Version 3
|
||||
@ Yaël Moussouni
|
||||
@ Unistra, P&E, MSc1-MoFP
|
||||
@ Observatory of Strasbourg (Intern)
|
||||
"""
|
||||
|
||||
import numpy as np
|
||||
import amuse.units.units as u
|
||||
|
||||
def rotation(stars, params):
|
||||
N = params["N_stars"] + np.int32(np.round(params["N_stars"] * params["binary_fraction"]))
|
||||
stars.X_v = np.random.uniform(0, 10, N) | u.km * u.s**(-1)
|
||||
p = np.random.uniform(0, 1, N)
|
||||
stars.X_vsini = stars.X_v * np.sqrt(2*p-p**2)
|
||||
return stars
|
||||
|
||||
def X_emission(stars, params):
|
||||
for i in range(len(stars)):
|
||||
if stars[i].temperature.value_in(u.K) > 7300: # O B A
|
||||
stars[i].X_luminosity = params["X_coefficient_OBA"] * stars[i].luminosity.in_(u.erg * u.s**(-1))
|
||||
elif stars[i].temperature.value_in(u.K) < 6000: # G K M
|
||||
stars[i].X_luminosity = params["X_coefficient_GKM"] * (stars[i].X_vsini.value_in(u.km * u.s**(-1)))**(1.9) | u.erg * u.s**(-1)
|
||||
else: # F
|
||||
stars[i].X_luminosity = 0
|
||||
return stars
|
||||
44
COSMIC/source/COSMIC_v3_evolve.py
Normal file
44
COSMIC/source/COSMIC_v3_evolve.py
Normal file
@@ -0,0 +1,44 @@
|
||||
"""
|
||||
* COSMIC - EVOLVE
|
||||
* Version 3
|
||||
@ Yaël Moussouni
|
||||
@ Unistra, P&E, MSc1-MoFP
|
||||
@ Observatory of Strasbourg (Intern)
|
||||
"""
|
||||
|
||||
import numpy as np
|
||||
import amuse.units.units as u
|
||||
import COSMIC_v3_output as output
|
||||
import COSMIC_v3_emission as emission
|
||||
|
||||
def stellar_gravity(codes, stars, channels, params, save_stars = False):
|
||||
"""
|
||||
Evolve a model with both gravity and stellar evolution.
|
||||
"""
|
||||
for t in params["output_times"]:
|
||||
print("\033[36m"+"t: "+"\033[0m"+"{:02.2f} Myr/{:02.2f} Myr".format(t.value_in(u.Myr),np.max(params["output_times"].value_in(u.Myr))))
|
||||
codes["g"].evolve_model(t)
|
||||
channels.copy()
|
||||
if save_stars: output.save_stars(stars, params, t.value_in(u.Myr))
|
||||
|
||||
print("\033[36m"+"Simulation completed"+"\033[0m")
|
||||
return 0
|
||||
|
||||
def stellar_gravity_binaries(codes, stars, binaries, channels, params, save_stars = False, save_binaries = False, compute_X_emission = False):
|
||||
"""
|
||||
Evolve a model with both gravity and stellar evolution.
|
||||
"""
|
||||
for t in params["output_times"]:
|
||||
print("\033[36m"+"t: "+"\033[0m"+"{:02.2f} Myr/{:02.2f} Myr".format(t.value_in(u.Myr),np.max(params["output_times"].value_in(u.Myr))))
|
||||
codes["b"].evolve_model(t)
|
||||
channels.copy()
|
||||
if compute_X_emission:
|
||||
stars = emission.rotation(stars, params)
|
||||
stars = emission.X_emission(stars, params)
|
||||
if save_stars: output.save_stars(stars, params, t.value_in(u.Myr))
|
||||
if save_binaries: output.save_binaries(binaries, params, t.value_in(u.Myr))
|
||||
|
||||
print("\033[36m"+"Simulation completed"+"\033[0m")
|
||||
return codes, stars, channels
|
||||
|
||||
|
||||
0
COSMIC/source/COSMIC_v3_galaxy.py
Normal file
0
COSMIC/source/COSMIC_v3_galaxy.py
Normal file
193
COSMIC/source/COSMIC_v3_init.py
Normal file
193
COSMIC/source/COSMIC_v3_init.py
Normal file
@@ -0,0 +1,193 @@
|
||||
"""
|
||||
* COSMIC - INIT
|
||||
* Version 3
|
||||
@ Yaël Moussouni
|
||||
@ Unistra, P&E, MSc1-MoFP
|
||||
@ Observatory of Strasbourg (Intern)
|
||||
"""
|
||||
|
||||
import numpy as np
|
||||
import amuse.units.units as u
|
||||
|
||||
import COSMIC_v3_galaxy as galaxy
|
||||
|
||||
from amuse.units import nbody_system
|
||||
from amuse.ic.kingmodel import new_king_model
|
||||
from amuse.ic.salpeter import new_salpeter_mass_distribution
|
||||
# from amuse.community.huayno.interface import Huayno # FIXME DOES NOT WORK
|
||||
from amuse.community.ph4.interface import Ph4
|
||||
from amuse.community.seba.interface import SeBa
|
||||
from amuse.couple.bridge import Bridge
|
||||
from amuse.datamodel.particles import Channels
|
||||
from amuse.datamodel import Particles
|
||||
|
||||
# def IMF_Besancon(M, alpha_1=1.6, alpha_2=3.0):
|
||||
# return (M.value_in(u.MSun))**(alpha_1-1) * ((M.value_in(u.MSun))<1) + (((M.value_in(u.MSun))-1)**(alpha_2-1) + 1) * ((M.value_in(u.MSun))>=1)
|
||||
|
||||
# def Besancon_disk(params):
|
||||
# """
|
||||
# Generate two IMF of stars and binaries
|
||||
# """
|
||||
# M_1 = []
|
||||
# M_2 = []
|
||||
# N_min = 0
|
||||
# N_max = IMF_Besancon(params["M_max_besancon"], params["a_besancon_1"], params["a_besancon_2"])
|
||||
# while len(M_1) < params["N_stars"]:
|
||||
# X = np.random.uniform(params["M_min_besancon"].value_in(u.MSun), params["M_max_besancon"].value_in(u.MSun))|u.MSun
|
||||
# Y = np.random.uniform(N_min, N_max)
|
||||
# if Y > IMF_Besancon(X, params["a_besancon_1"], params["a_besancon_2"]):
|
||||
# M_1.append(X)
|
||||
# while len(M_2) < params["N_stars"] * params["binary_fraction"]:
|
||||
# X = np.random.uniform(params["M_min_besancon"].value_in(u.MSun), params["M_max_besancon"].value_in(u.MSun))|u.MSun
|
||||
# Y = np.random.uniform(N_min, N_max)
|
||||
# if Y > IMF_Besancon(X, params["a_besancon_1"], params["a_besancon_2"]):
|
||||
# M_2.append(X)
|
||||
# return M_1, M_2
|
||||
|
||||
def orbital_parameters(params, m_tot):
|
||||
x_0 = params["mean_period"] * np.log(2)
|
||||
sigma_0 = params["std_period"] * np.log(2)
|
||||
T = np.random.lognormal(mean = x_0, sigma = sigma_0)
|
||||
a = (T**2 * u.constants.G.value_in(u.au**3*u.day**(-2)*u.MSun**(-1)) * m_tot.value_in(u.MSun) / (4*np.pi**2) )**(1/3) | u.au
|
||||
e = 1
|
||||
return a, e
|
||||
|
||||
def king_salpeter(params):
|
||||
"""
|
||||
Create a cluster of N stars, with a King's law of parameter W0, with a (virial) radius R, stellar masses following a Salpeter law ranging between M_min and M_max with exponent a_salpeter.
|
||||
"""
|
||||
M_stars = new_salpeter_mass_distribution(params["N_stars"], mass_min=params["M_min_salpeter"], mass_max=params["M_max_salpeter"], alpha=params["a_salpeter"])
|
||||
converter = nbody_system.nbody_to_si(M_stars.sum(), params["R0_king"])
|
||||
stars = new_king_model(params["N_stars"], params["W0_king"], converter)
|
||||
stars.mass = M_stars
|
||||
stars.zams_mass = M_stars
|
||||
return stars, converter
|
||||
|
||||
def king_salpeter_binaries(params):
|
||||
"""
|
||||
|
||||
"""
|
||||
M_primary = new_salpeter_mass_distribution(params["N_stars"], mass_min=params["M_min_salpeter"], mass_max=params["M_max_salpeter"], alpha=params["a_salpeter"])
|
||||
M_secondary = new_salpeter_mass_distribution(np.int32(np.round(params["N_stars"]*params["binary_fraction"])), mass_min=params["M_min_salpeter"], mass_max=params["M_max_salpeter"], alpha=params["a_salpeter"])
|
||||
|
||||
M_stars = np.concatenate([M_primary, M_secondary])
|
||||
N_binaries = len(M_secondary)
|
||||
converter = nbody_system.nbody_to_si(M_stars.sum(), params["R0_king"])
|
||||
stars_primary = new_king_model(params["N_stars"], params["W0_king"], converter)
|
||||
stars_primary.mass = M_primary
|
||||
stars_primary.zams_mass = M_primary
|
||||
|
||||
stars_secondary = Particles(N_binaries)
|
||||
for i in range(N_binaries):
|
||||
stars_secondary[i].mass = M_secondary[i]
|
||||
stars_secondary[i].radius = 0|u.m
|
||||
stars_secondary[i].vx = stars_primary[i].vx
|
||||
stars_secondary[i].vy = stars_primary[i].vy
|
||||
stars_secondary[i].vz = stars_primary[i].vz
|
||||
stars_secondary[i].x = stars_primary[i].x
|
||||
stars_secondary[i].y = stars_primary[i].y
|
||||
stars_secondary[i].z = stars_primary[i].z
|
||||
stars_secondary[i].zams_mass = M_secondary[i]
|
||||
|
||||
stars = Particles()
|
||||
binaries = Particles(N_binaries)
|
||||
|
||||
stars.add_particles(stars_primary)
|
||||
stars.add_particles(stars_secondary)
|
||||
|
||||
stars.ra = 0 | u.deg
|
||||
stars.dec = 0 | u.deg
|
||||
stars.X_v = 0 | u.km * u.s**(-1)
|
||||
stars.X_vsini = 0 | u.km * u.s**(-1)
|
||||
stars.X_temperature_0 = 0 | u.kilo(u.eV)
|
||||
stars.X_temperature_1 = 0 | u.kilo(u.eV)
|
||||
stars.X_luminosity = 0 | u.erg * u.s**(-1)
|
||||
|
||||
if N_binaries == 0:
|
||||
binaries.child1 = [0]
|
||||
binaries.child2 = [0]
|
||||
binaries.mass1 = 0
|
||||
binaries.mass2 = 0
|
||||
binaries.mass_tot = 0
|
||||
else:
|
||||
binaries.child1 = list(stars_primary[:N_binaries])
|
||||
binaries.child2 = list(stars_secondary)
|
||||
binaries.mass1 = list(stars_primary[:N_binaries].mass)
|
||||
binaries.mass2 = list(stars_secondary.mass.in_(u.kg))
|
||||
binaries.mass_tot = binaries.mass1 + binaries.mass2
|
||||
|
||||
for i in range(N_binaries):
|
||||
semi_major_axis, eccentricity = orbital_parameters(params, binaries[i].mass_tot)
|
||||
binaries[i].semi_major_axis = semi_major_axis
|
||||
binaries[i].eccentricity = eccentricity
|
||||
return stars, binaries, converter
|
||||
|
||||
|
||||
def gravity_stellar_bridge(converter, params):
|
||||
gravity = Ph4(converter, number_of_workers=params["workers_gravity"]) # TODO A CHANGER SI BESOIN
|
||||
stellar = SeBa(number_of_worker=params["workers_stellar"])
|
||||
bridge = Bridge()
|
||||
codes = {"g":gravity, "s":stellar, "b":bridge}
|
||||
return codes
|
||||
|
||||
def create_channels():
|
||||
channels = Channels()
|
||||
return channels
|
||||
|
||||
def generate_galaxy(stars, params):
|
||||
galaxy_model = galaxy.MilkyWay_AMUSE()
|
||||
vc = galaxy_model.vel_circ(stars.center_of_mass().length())
|
||||
stars.x += params["cluster_position_x"]
|
||||
stars.y += params["cluster_position_y"]
|
||||
stars.z += params["cluster_position_z"]
|
||||
phi = np.arctan2(stars.center_of_mass().y, stars.center_of_mass().x)
|
||||
stars.vx += - vc * np.sin(phi)
|
||||
stars.vy += vc * np.cos(phi)
|
||||
return stars, galaxy_model
|
||||
|
||||
def add_stars(codes, stars):
|
||||
codes["g"].particles.add_particles(stars)
|
||||
codes["s"].particles.add_particles(stars)
|
||||
return codes
|
||||
|
||||
def add_binaries(codes, stars, binaries, channels):
|
||||
codes["s"].binaries.add_particles(binaries)
|
||||
channels.add_channel(codes["s"].binaries.new_channel_to(stars))
|
||||
return codes, channels
|
||||
|
||||
def commit(codes, stars, channels, params):
|
||||
codes["s"].set_metallicity(params["metallicity_stellar"])
|
||||
codes["s"].commit_particles()
|
||||
codes["g"].commit_particles()
|
||||
# codes["g"].initialize_code() # NOT REQUIRED WITH Ph4
|
||||
|
||||
codes["b"].add_system(codes["g"])
|
||||
codes["b"].add_system(codes["s"])
|
||||
|
||||
codes["b"].synchronize_model()
|
||||
codes["b"].timestep = params["timestep"]
|
||||
|
||||
codes["b"].channels.add_channel(codes["s"].particles.new_channel_to(codes["g"].particles, attributes=["mass", "radius"]))
|
||||
|
||||
channels.add_channel(codes["s"].particles.new_channel_to(stars))
|
||||
channels.add_channel(codes["g"].particles.new_channel_to(stars))
|
||||
return codes, channels
|
||||
|
||||
def commit_with_potential(codes, stars, channels, galaxy_model, params):
|
||||
codes["s"].set_metallicity(params["metallicity_stellar"])
|
||||
codes["s"].commit_particles()
|
||||
codes["g"].commit_particles()
|
||||
# codes["g"].initialize_code() # NOT REQUIRED WITH Ph4
|
||||
|
||||
codes["b"].add_system(codes["g"], (galaxy_model,))
|
||||
codes["b"].add_system(codes["s"])
|
||||
|
||||
codes["b"].synchronize_model()
|
||||
codes["b"].timestep = params["timestep"]
|
||||
|
||||
codes["b"].channels.add_channel(codes["s"].particles.new_channel_to(codes["g"].particles, attributes=["mass", "radius"]))
|
||||
|
||||
channels.add_channel(codes["s"].particles.new_channel_to(stars))
|
||||
channels.add_channel(codes["g"].particles.new_channel_to(stars))
|
||||
return codes, channels
|
||||
|
||||
20
COSMIC/source/COSMIC_v3_output.py
Normal file
20
COSMIC/source/COSMIC_v3_output.py
Normal file
@@ -0,0 +1,20 @@
|
||||
"""
|
||||
* COSMIC - SAVE
|
||||
* Version 3
|
||||
@ Yaël Moussouni
|
||||
@ Unistra, P&E, MSc1-MoFP
|
||||
@ Observatory of Strasbourg (Intern)
|
||||
"""
|
||||
|
||||
|
||||
import numpy as np
|
||||
|
||||
from amuse.io.base import write_set_to_file
|
||||
|
||||
def save_stars(stars, params, t=0):
|
||||
write_set_to_file(set=stars, filename=params["out_directory"]+params["filename"]+"_stars_{:04d}_Myr.{}".format(np.int32(t), params["format_type"]), format=params["format_type"])
|
||||
return 0
|
||||
|
||||
def save_binaries(binaries, params, t=0):
|
||||
write_set_to_file(set=binaries, filename=params["out_directory"]+params["filename"]+"_binaries_{:04d}_Myr.{}".format(np.int32(t), params["format_type"]), format=params["format_type"])
|
||||
return 0
|
||||
Reference in New Issue
Block a user