def main(Ndisk, Mstar, Mdisk, Rin, Rout, t_end, Nray, x, y, z):
time = 0 | units.Myr
supernova_IIp = Supernova_IIp(10|units.day)
efficiency_factor = 0.1
Rsn = efficiency_factor * (x**2 + y**2 + z**2)**0.5
supernova = Particle()
supernova.position = (x.value_in(units.parsec),
y.value_in(units.parsec),
z.value_in(units.parsec)) |units.parsec
supernova.position *= efficiency_factor
supernova_IIp.particles.add_particle(supernova)
supernova_IIp.evolve_model(time)
supernova.luminosity = efficiency_factor**2 * supernova.luminosity
supernova.xion = 0.0
supernova.u = (10**51 | units.erg)/(10|units.MSun)
stellar = SeBa()
star = Particle()
star.mass = Mstar
star.position = (0,0,0) | units.AU
star.velocity = (0,0,0) | units.kms
stellar.particles.add_particle(star)
stellar.evolve_model(1|units.Myr)
star.luminosity = stellar.particles[0].luminosity/(20. | units.eV)
star.temperature = stellar.particles[0].temperature
stellar.stop()
star.u = (9. |units.kms)**2
star.xion = 0.0
print star
print "M=", Mdisk/Mstar
converter=nbody_system.nbody_to_si(Mstar, 1 | units.AU)
disk = ProtoPlanetaryDisk(Ndisk, convert_nbody=converter,
Rmin=Rin.value_in(units.AU),
Rmax=Rout.value_in(units.AU),
q_out=25.0, discfraction=Mdisk/Mstar).result
#### q_out=2.0, discfraction=Mdisk/Mstar).result
print disk.x.max().in_(units.AU)
print disk.mass.sum().in_(units.MSun)
print disk.u.max().in_(units.kms**2)
print disk.mass.min().in_(units.MSun)
disk.flux = 0. | units.s**-1
disk.xion = 0.0
dt = t_end/1000.
hydro = Fi(converter)
hydro.parameters.use_hydro_flag=True
hydro.parameters.radiation_flag=False
hydro.parameters.self_gravity_flag=True
hydro.parameters.gamma=1.
hydro.parameters.isothermal_flag=True
# Non-isothermal: lowest temperature remains constat at 20K
# hydro.parameters.gamma=1.66667
# hydro.parameters.isothermal_flag=False
hydro.parameters.integrate_entropy_flag=False
hydro.parameters.timestep=0.5 | units.hour #0.125 | units.day
# hydro.parameters.verbosity=99
hydro.parameters.epsilon_squared=0.1 | units.AU**2
hydro.parameters.courant=0.2
hydro.parameters.artificial_viscosity_alpha = 0.1
hydro.gas_particles.add_particles(disk)
hydro.dm_particles.add_particle(star)
hydro_to_disk = hydro.gas_particles.new_channel_to(disk)
hydro_to_star = hydro.dm_particles.new_channel_to(star.as_set())
disk_to_hydro = disk.new_channel_to(hydro.gas_particles)
star_to_hydro = star.as_set().new_channel_to(hydro.dm_particles)
hydro.evolve_model(1|units.hour)
hydro_to_disk.copy()
hydro_to_star.copy()
radiative = SPHRay(redirection="file",
number_of_workers=4)#, debugger="gdb")
radiative.parameters.number_of_rays=Nray/dt
print dt.in_(units.yr)
radiative.parameters.default_spectral_type=-3.
radiative.parameters.box_size=10000. | units.AU
radiative.parameters.ionization_temperature_solver=2
print radiative.parameters
# radiative.src_particles.add_particle(star)
radiative.src_particles.add_particle(supernova)
radiative.gas_particles.add_particles(disk)
gas_to_rad = disk.new_channel_to(radiative.gas_particles)
rad_to_gas = radiative.gas_particles.new_channel_to(disk)
print "Before"
print "Luminosity:", radiative.src_particles.luminosity
print "min ionization:", radiative.gas_particles.xion.min()
print "average Xion:", radiative.gas_particles.xion.mean()
print "max ionization:", radiative.gas_particles.xion.max()
print "min u:", radiative.gas_particles.u.min()
print "average u:", radiative.gas_particles.u.mean()
print "max u:", radiative.gas_particles.u.max()
Tmean = [] | units.K
Tmin = [] | units.K
Tmax = [] | units.K
t = [] | units.day
while radiative.model_time<t_end:
supernova = update_source_particle(radiative, time+0.5*dt, supernova,
efficiency_factor, supernova_IIp)
radiative.evolve_model(time+0.5*dt)
print "RT done at time:", time.in_(units.day)
rad_to_gas.copy()
disk_to_hydro.copy()
star_to_hydro.copy()
hydro.evolve_model(time + dt)
hydro_to_disk.copy()
hydro_to_star.copy()
supernova = update_source_particle(radiative, time+dt, supernova,
efficiency_factor, supernova_IIp)
radiative.evolve_model(time+dt)
print "RT done at time:", time.in_(units.day)
rad_to_gas.copy()
time += dt
print_diagnostics(time, supernova, disk)
Temperature = mu() / constants.kB * disk.u
t.append(time)
Tmean.append(Temperature.mean())
Tmin.append(Temperature.min())
Tmax.append(Temperature.max())
#write_set_to_file(disk, "disk_irradiation.amuse", "amuse")
print "timescale:", (disk.mass.sum().value_in(units.amu) \
/ ((Rout/Rsn)**2*supernova.luminosity)).in_(units.yr)
print "scaleheight:", abs(disk.z.value_in(units.AU)).mean()
#pyplot.hist2d(abs(disk.x.value_in(units.AU)), abs(numpy.log10(Temperature.value_in(units.K))), bins=200)
# pyplot.hist2d(abs(disk.x.value_in(units.AU)), abs(disk.z.value_in(units.AU)), bins=200)
#,norm=LogNorm())
#, Temperature.in_(units.K))
# pyplot.tripcolor(abs(disk.x.value_in(units.AU)), abs(disk.y.value_in(units.AU)), Temperature.in_(units.K))
#pyplot.hist(abs(disk.x.value_in(units.AU)), 100)
# pyplot.show()
print_diagnostics(time, supernova, disk)
#plot_ionization_fraction(disk.position, disk.xion)
# plot_ionization_fraction(disk.z, disk.u.value_in(units.kms**2))
# plot_ionization_fraction(disk.x, disk.u.value_in(units.kms**2))
radiative.stop()
plot_temperature(t, Tmin, Tmean, Tmax)
def main(Ndisk, Mstar, Mdisk, Rin, Rout, t_end, Nray, x, y, z):
time = 0 | units.Myr
supernova_IIp = Supernova_IIp(10|units.day)
efficiency_factor = 0.1
Rsn = efficiency_factor * (x**2 + y**2 + z**2)**0.5
supernova=Particle()
supernova.position = (x.value_in(units.parsec),
y.value_in(units.parsec),
z.value_in(units.parsec)) |units.parsec
supernova.position *= efficiency_factor
supernova.luminosity = efficiency_factor**2 * supernova_IIp.luminosity_at_time(time)/(20.|units.eV)
# supernova.flux = supernova.luminosity
supernova.xion = 0.0
supernova.u = (10**51 | units.erg)/(10|units.MSun)
stellar = SeBa()
star = Particle()
star.mass = Mstar
star.position = (0,0,0) | units.AU
star.velocity = (0,0,0) | units.kms
stellar.particles.add_particle(star)
stellar.evolve_model(1|units.Myr)
star.luminosity = stellar.particles[0].luminosity/(20. | units.eV)
star.temperature = stellar.particles[0].temperature
stellar.stop()
star.u = (9. |units.kms)**2
star.xion = 0.0
print star
print "M=", Mdisk/Mstar
converter=nbody_system.nbody_to_si(Mstar, 1 | units.AU)
disk = ProtoPlanetaryDisk(Ndisk, convert_nbody=converter,
Rmin=Rin.value_in(units.AU),
Rmax=Rout.value_in(units.AU),
q_out=25.0, discfraction=Mdisk/Mstar).result
#### q_out=2.0, discfraction=Mdisk/Mstar).result
print disk.x.max().in_(units.AU)
print disk.mass.sum().in_(units.MSun)
print disk.u.max().in_(units.kms**2)
print disk.mass.min().in_(units.MSun)
disk.flux = 0. | units.s**-1
disk.xion = 0.0
dt = t_end/1000.
hydro = Fi(converter)
hydro.parameters.use_hydro_flag=True
hydro.parameters.radiation_flag=False
hydro.parameters.self_gravity_flag=True
hydro.parameters.gamma=1.
hydro.parameters.isothermal_flag=True
# Non-isothermal: lowest temperature remains constat at 20K
# hydro.parameters.gamma=1.66667
# hydro.parameters.isothermal_flag=False
hydro.parameters.integrate_entropy_flag=False
hydro.parameters.timestep=0.5 | units.hour #0.125 | units.day
# hydro.parameters.verbosity=99
hydro.parameters.epsilon_squared=0.1 | units.AU**2
hydro.parameters.courant=0.2
hydro.parameters.artificial_viscosity_alpha = 0.1
hydro.gas_particles.add_particles(disk)
hydro.dm_particles.add_particle(star)
hydro_to_disk = hydro.gas_particles.new_channel_to(disk)
hydro_to_star = hydro.dm_particles.new_channel_to(star.as_set())
disk_to_hydro = disk.new_channel_to(hydro.gas_particles)
star_to_hydro = star.as_set().new_channel_to(hydro.dm_particles)
hydro.evolve_model(1|units.hour)
hydro_to_disk.copy()
hydro_to_star.copy()
radiative = SPHRay(redirection="file", number_of_workers=4)#, debugger="gdb")
radiative.parameters.number_of_rays=Nray/dt
print dt.in_(units.yr)
radiative.parameters.default_spectral_type=-3.
radiative.parameters.box_size=10000. | units.AU
radiative.parameters.ionization_temperature_solver=2
print radiative.parameters
# radiative.src_particles.add_particle(star)
radiative.src_particles.add_particle(supernova)
radiative.gas_particles.add_particles(disk)
gas_to_rad = disk.new_channel_to(radiative.gas_particles)
rad_to_gas = radiative.gas_particles.new_channel_to(disk)
print "Before"
print "Luminosity:", radiative.src_particles.luminosity
print "min ionization:", radiative.gas_particles.xion.min()
print "average Xion:", radiative.gas_particles.xion.mean()
print "max ionization:", radiative.gas_particles.xion.max()
print "min u:", radiative.gas_particles.u.min()
print "average u:", radiative.gas_particles.u.mean()
print "max u:", radiative.gas_particles.u.max()
Tmean = [] | units.K
Tmin = [] | units.K
Tmax = [] | units.K
t = [] | units.day
while radiative.model_time<t_end:
supernova = update_source_particle(radiative, time+0.5*dt, supernova, efficiency_factor, supernova_IIp)
radiative.evolve_model(time+0.5*dt)
print "RT done at time:", time.in_(units.day)
rad_to_gas.copy()
disk_to_hydro.copy()
star_to_hydro.copy()
hydro.evolve_model(time + dt)
hydro_to_disk.copy()
hydro_to_star.copy()
supernova = update_source_particle(radiative, time+dt, supernova, efficiency_factor, supernova_IIp)
radiative.evolve_model(time+dt)
print "RT done at time:", time.in_(units.day)
rad_to_gas.copy()
time += dt
print_diagnostics(time, supernova, disk)
Temperature = mu() / constants.kB * disk.u
t.append(time)
Tmean.append(Temperature.mean())
Tmin.append(Temperature.min())
Tmax.append(Temperature.max())
#write_set_to_file(disk, "disk_irradiation.amuse", "amuse")
print "timescale:", (disk.mass.sum().value_in(units.amu)/((Rout/Rsn)**2*supernova.luminosity)).in_(units.yr)
print "scaleheight:", abs(disk.z.value_in(units.AU)).mean()
#pyplot.hist2d(abs(disk.x.value_in(units.AU)), abs(numpy.log10(Temperature.value_in(units.K))), bins=200)
# pyplot.hist2d(abs(disk.x.value_in(units.AU)), abs(disk.z.value_in(units.AU)), bins=200)
#,norm=LogNorm())
#, Temperature.in_(units.K))
# pyplot.tripcolor(abs(disk.x.value_in(units.AU)), abs(disk.y.value_in(units.AU)), Temperature.in_(units.K))
#pyplot.hist(abs(disk.x.value_in(units.AU)), 100)
# pyplot.show()
print_diagnostics(time, supernova, disk)
#plot_ionization_fraction(disk.position, disk.xion)
# plot_ionization_fraction(disk.z, disk.u.value_in(units.kms**2))
# plot_ionization_fraction(disk.x, disk.u.value_in(units.kms**2))
radiative.stop()
plot_temperature(t, Tmin, Tmean, Tmax)
def disk_in_cluster(N_stars, N_gasParticles, W0):
#set up protoplanetary disk
Mdisk = 1.|units.MSun
Rdisk = 100.|units.AU # HD 106906 b is at 700 AU
Rmin, Rmax = 1.|units.AU, Rdisk
converter_disk = nbody_system.nbody_to_si(Mdisk, Rdisk)
disk_particles = ProtoPlanetaryDisk(N_gasParticles, convert_nbody=converter_disk, densitypower=1.5, Rmin=Rmin.value_in(units.AU), Rmax=Rmax.value_in(units.AU), q_out=1.0, discfraction=1.0).result
hydro = Fi(converter_disk, mode='openmp')
hydro.gas_particles.add_particles(disk_particles)
hydro_to_framework = hydro.gas_particles.new_channel_to(disk_particles)
framework_to_hydro = disk_particles.new_channel_to(hydro.gas_particles)
#set up star cluster
Mmin, Mmax = 0.1|units.MSun, 100.|units.MSun
Rvir = 1.|units.parsec
masses = new_kroupa_mass_distribution(N_stars, Mmax)
Mtot_init = masses.sum()
converter_cluster = nbody_system.nbody_to_si(Mtot_init, Rvir)
stars = new_king_model(N_stars, W0, convert_nbody=converter_cluster)
stars.mass = masses
dist_diff = 100. #|units.parsec
magic_index = -1
#put the disk around star closest to 1 solar mass
for i, star in enumerate(stars):
star_x = star.position.value_in(units.parsec)[0]
star_y = star.position.value_in(units.parsec)[1]
star_z = star.position.value_in(units.parsec)[2]
star_dist = np.sqrt(star_x**2 + star_y**2 + star_z**2)
i_diff = np.abs(star_dist - 1.0)
if i_diff < dist_diff:
magic_index = i
dist_diff = i_diff
for gas_particle in disk_particles:
gas_particle.position += stars[magic_index].position
gravitating_bodies = ParticlesSuperset([stars, disk_particles])
gravity = Hermite(converter_cluster)
gravity.particles.add_particles(gravitating_bodies)
gravity_to_framework = gravity.particles.new_channel_to(gravitating_bodies)
framework_to_gravity = gravitating_bodies.new_channel_to(gravity.particles)
combined = bridge.Bridge()
combined.add_system(gravity, (hydro,))
combined.add_system(hydro, (gravity,))
tend, dt = 10.|units.Myr, 0.005|units.Myr
sim_times_unitless = np.arange(0., tend.value_in(units.Myr)+dt.value_in(units.Myr), dt.value_in(units.Myr))
sim_times = [ t|units.Myr for t in sim_times_unitless ]
plt.rc('font', family = 'serif')
cmap = cm.get_cmap('nipy_spectral')
rvals, zvals = [], []
t0 = time.time()
for j, t in enumerate(sim_times):
if j%1 == 0:
print('')
print('simulation time: ', t)
print('wall time: %.03f minutes'%((time.time()-t0)/60.))
stars = gravity.particles[:N_stars]
gas = gravity.particles[N_stars:]
stars_x = [ stars.position[i].value_in(units.parsec)[0] for i in range(len(stars)) ]
stars_y = [ stars.position[i].value_in(units.parsec)[1] for i in range(len(stars)) ]
gas_x = [ gas.position[i].value_in(units.parsec)[0] for i in range(len(gas)) ]
gas_y = [ gas.position[i].value_in(units.parsec)[1] for i in range(len(gas)) ]
plt.figure()
colors = np.log10(stars.mass.value_in(units.MSun))
sc = plt.scatter(stars_x, stars_y, c=colors, s=1, alpha=0.5, label='Stars')
gas_sc = plt.scatter(gas_x, gas_y, c='r', s=1, alpha=0.8, label='Protoplanetary Disk')
cbar = plt.colorbar(sc)
cbar.set_label(r'$\log_{10}(M_{\star}/M_{\odot})$', fontsize=14)
plt.annotate(r'$M_{\mathrm{cluster}} = %.03f \, M_{\odot}$'%(Mtot_init.value_in(units.MSun)), xy=(0.65, 0.15), xycoords='axes fraction', fontsize=8)
plt.annotate(r'$t = %.02f$ Myr'%(t.value_in(units.Myr)), xy=(0.65, 0.1), xycoords='axes fraction', fontsize=8)
plt.xlim(-4.*Rvir.value_in(units.parsec), 4.*Rvir.value_in(units.parsec))
plt.ylim(-4.*Rvir.value_in(units.parsec), 4.*Rvir.value_in(units.parsec))
plt.gca().set_aspect('equal')
plt.xlabel('$x$ (pc)', fontsize=14)
plt.ylabel('$y$ (pc)', fontsize=14)
plt.legend(loc='upper left', fontsize=8)
plt.title(r'King Model, $W_{0} = %.01f$'%(W0), fontsize=14)
plt.savefig('kingmodel_%s.png'%(str(j).rjust(5, '0')))
plt.close()
combined.evolve_model(t)
combined.stop()
return 0
