def main(N=1000, Lstar=100| units.LSun, boxsize=10| units.parsec,
rho=1.0| (units.amu/units.cm**3), t_end=0.1|units.Myr, n_steps=10):
ionization_fraction = 0.0
internal_energy = (9. |units.kms)**2
source=Particles(1)
source.position = (0, 0, 0) |units.parsec
source.flux = Lstar/(20. | units.eV)
source.luminosity = Lstar/(20. | units.eV)
source.rho = rho
source.xion = ionization_fraction
source.u = internal_energy
converter=nbody_system.nbody_to_si(1|units.MSun, boxsize)
ism = ProtoPlanetaryDisk(N, convert_nbody=converter,
densitypower=1.5,
Rmin=0.1,
Rmax=1,
q_out=1.0,
discfraction=1.0).result
ism = ism.select(lambda r: r.length()<0.5*boxsize,["position"])
gamma=5./3.
mu=1.| units.amu
Tinit = 10000|units.K
ism.u = 1/(gamma-1)*constants.kB * Tinit/mu
ism.rho = rho
ism.flux = 0. | units.s**-1
ism.xion = ionization_fraction
ism.h_smooth = 0 | units.AU
rad = SimpleXSplitSet(redirect="none")
# rad = SimpleX()
# rad = SPHRay()
rad.parameters.box_size=1.001*boxsize
rad.parameters.timestep=0.001 | units.Myr
rad.src_particles.add_particle(source)
rad.gas_particles.add_particles(ism)
channel_to_local_gas = rad.gas_particles.new_channel_to(ism)
write_set_to_file(ism, "rad.hdf5", 'hdf5')
time = 0.0 | t_end.unit
dt = t_end/float(n_steps)
while time<t_end:
time += dt
rad.evolve_model(time)
channel_to_local_gas.copy_attributes(["xion",])
write_set_to_file(ism, "rad.hdf5", 'hdf5')
print "Time=", time
print "min ionization:", rad.gas_particles.xion.min()
print "average Xion:", rad.gas_particles.xion.mean()
print "max ionization:", rad.gas_particles.xion.max()
rad.stop()
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 main(N=1000,
Lstar=100 | units.LSun,
boxsize=10 | units.parsec,
rho=1.0 | (units.amu / units.cm**3),
t_end=0.1 | units.Myr,
n_steps=10):
ionization_fraction = 0.0
internal_energy = (9. | units.kms)**2
source = Particles(1)
source.position = (0, 0, 0) | units.parsec
source.flux = Lstar / (20. | units.eV)
source.luminosity = Lstar / (20. | units.eV)
source.rho = rho
source.xion = ionization_fraction
source.u = internal_energy
converter = nbody_system.nbody_to_si(1 | units.MSun, boxsize)
ism = ProtoPlanetaryDisk(N,
convert_nbody=converter,
densitypower=1.5,
Rmin=0.1,
Rmax=1,
q_out=1.0,
discfraction=1.0).result
ism = ism.select(lambda r: r.length() < 0.5 * boxsize, ["position"])
gamma = 5. / 3.
mu = 1. | units.amu
Tinit = 10000 | units.K
ism.u = 1 / (gamma - 1) * constants.kB * Tinit / mu
ism.rho = rho
ism.flux = 0. | units.s**-1
ism.xion = ionization_fraction
ism.h_smooth = 0 | units.AU
rad = SimpleXSplitSet(redirect="none")
# rad = SimpleX()
# rad = SPHRay()
rad.parameters.box_size = 1.001 * boxsize
rad.parameters.timestep = 0.001 | units.Myr
rad.src_particles.add_particle(source)
rad.gas_particles.add_particles(ism)
channel_to_local_gas = rad.gas_particles.new_channel_to(ism)
write_set_to_file(ism, "rad.hdf5", 'hdf5')
time = 0.0 | t_end.unit
dt = t_end / float(n_steps)
while time < t_end:
time += dt
rad.evolve_model(time)
channel_to_local_gas.copy_attributes([
"xion",
])
write_set_to_file(ism, "rad.hdf5", 'hdf5')
print("Time=", time)
print("min ionization:", rad.gas_particles.xion.min())
print("average Xion:", rad.gas_particles.xion.mean())
print("max ionization:", rad.gas_particles.xion.max())
rad.stop()
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)
