def main():
"Test class with an IMF"
import sys
import numpy
from amuse.units import units
numpy.random.seed(11)
try:
from amuse_masc import make_a_star_cluster
use_masc = True
except ImportError:
use_masc = False
if len(sys.argv) > 1:
from amuse.io import read_set_from_file
stars = read_set_from_file(sys.argv[1], "amuse")
elif use_masc:
stars = make_a_star_cluster.new_cluster(number_of_stars=10001)
else:
from amuse.ic.salpeter import new_salpeter_mass_distribution
stars = Particles(10000)
stars.mass = new_salpeter_mass_distribution(len(stars))
print("Number of stars: %i" % (len(stars)))
code = StellarEvolutionCode(evo_code=SeBa)
code.particles.add_particles(stars)
print(code.parameters)
timestep = 0.2 | units.Myr
for step in range(10):
time = step * timestep
code.evolve_model(time)
print("Evolved to %s" % code.model_time.in_(units.Myr))
print("Most massive star: %s" % code.particles.mass.max())
def test16(self):
print "test evolution of 1000 star sampled over flattish IMF"
number_of_stars=1000
class notsorandom(object):
def random(self,N):
return numpy.array(range(N))/(N-1.)
def random_sample(self,N):
return numpy.array(range(N))/(N-1.)
masses = new_salpeter_mass_distribution(
number_of_stars,
mass_min = 0.1 | units.MSun,
mass_max = 100.0 | units.MSun,
alpha = -1.01,random=notsorandom()
)
stars=Particles(mass=masses)
instance=SSE()
instance.particles.add_particles(stars)
i=0
for p in instance.particles:
print i,p.mass,
p.evolve_for(13.2 | units.Gyr)
print p.mass
i+=1
instance.stop()
def test16(self):
print("test evolution of 1000 star sampled over flattish IMF")
number_of_stars = 1000
class notsorandom(object):
def random(self, N):
return numpy.array(range(N)) / (N - 1.)
def random_sample(self, N):
return numpy.array(range(N)) / (N - 1.)
masses = new_salpeter_mass_distribution(number_of_stars,
mass_min=0.1 | units.MSun,
mass_max=100.0 | units.MSun,
alpha=-1.01,
random=notsorandom())
stars = Particles(mass=masses)
instance = SSE()
instance.particles.add_particles(stars)
i = 0
for p in instance.particles:
p.evolve_for(13.2 | units.Gyr)
i += 1
instance.stop()
def __init__(self,
num_stars,
xoffset,
yoffset,
zoffset,
repopulate_every_run=True):
self.num_stars = num_stars
self.xoffset = xoffset
self.yoffset = yoffset
self.zoffset = zoffset
self.repopulate_every_run = repopulate_every_run
if repopulate_every_run is False:
# create nbody_converter thing?
convert_nbody = nbody_system.nbody_to_si(100.0 | units.MSun,
1 | units.parsec)
# instantiate plummer sphere
self.initial_plummer = new_plummer_sphere(self.num_stars,
convert_nbody)
self.initial_plummer.x += self.xoffset | units.lightyear
self.initial_plummer.y += self.yoffset | units.lightyear
self.initial_plummer.z += self.zoffset | units.lightyear
# provide mass distribution for stars
self.initial_plummer.mass = new_salpeter_mass_distribution(
self.num_stars)
self.plummer = None
def stellar_population(number_of_stars = 1000,min_mass=0.1, max_mass=125, alpha=-2.35):
"""
Generates a stellar population that follows the Salpeter mass function
"""
masses = new_salpeter_mass_distribution(number_of_stars, min_mass | units.MSun, max_mass | units.MSun, alpha = alpha)
return masses
def xslowtest16(self):
print "test full evolution of 1000 star sampled over flattish IMF"
number_of_stars=1000
from amuse.ic.salpeter import new_salpeter_mass_distribution
import numpy
class notsorandom(object):
def random(self,N):
return numpy.array(range(N))/(N-1.)
masses = new_salpeter_mass_distribution(
number_of_stars,
mass_min = 0.1 | units.MSun,
mass_max = 100.0 | units.MSun,
alpha = -1.01,random=notsorandom()
)
stars = Particles(mass=masses)
instance=EVtwin()
instance.parameters.maximum_number_of_stars=number_of_stars
instance.particles.add_particles(stars)
for p in instance.particles:
p.evolve_for(13.2 | units.Gyr)
def demo3(N):
salpeter_masses = new_salpeter_mass_distribution(N)
total_mass = salpeter_masses.sum()
convert_nbody = nbody_system.nbody_to_si(total_mass, 1.0 | units.parsec)
print convert_nbody.to_nbody(100 | units.Myr)
parts = new_plummer_model(N, convert_nbody)
parts.radius = 0. | units.RSun
parts.mass = salpeter_masses
parts.move_to_center()
gravity = PhiGRAPE(convert_nbody, use_gl=True)
eps = 0.001 | units.parsec
gravity.parameters.epsilon_squared = eps**2
gravity.particles.add_particles(parts)
stellar_evolution = SSE()
stellar_evolution.initialize_module_with_default_parameters()
stellar_evolution.particles.add_particles(parts)
return gravity, stellar_evolution
def create_stars(number_of_stars, size):
masses = new_salpeter_mass_distribution(number_of_stars, mass_min = 2|units.MSun)
converter = nbody_system.nbody_to_si(masses.sum(), size)
stars = new_plummer_model(number_of_stars, convert_nbody=converter)
stars.mass = masses
stars.zams_mass = masses
return stars, converter
def create_stars(number_of_stars, size):
masses = new_salpeter_mass_distribution(number_of_stars,
mass_min=2 | units.MSun)
converter = nbody_system.nbody_to_si(masses.sum(), size)
stars = new_plummer_model(number_of_stars, convert_nbody=converter)
stars.mass = masses
stars.zams_mass = masses
return stars, converter
def test5(self):
print("Test 5: testing user interface (SI units)")
numpy.random.seed(345672)
masses = new_salpeter_mass_distribution(1000)
self.assertEqual(len(masses), 1000)
self.assertAlmostEqual(masses.mean(), 0.334475937397 | units.MSun)
self.assertAlmostRelativeEqual(masses.mean(), SalpeterIMF().mass_mean(), 1)
self.assertAlmostEqual(masses.amin(), 0.10017909529 | units.MSun)
self.assertAlmostEqual(masses.amax(), 19.7132849297 | units.MSun)
def test5(self):
print "Test 5: testing user interface (SI units)"
numpy.random.seed(345672)
masses = new_salpeter_mass_distribution(1000)
self.assertEqual(len(masses), 1000)
self.assertAlmostEqual(masses.mean(), 0.334475937397 | units.MSun)
self.assertAlmostRelativeEqual(masses.mean(), SalpeterIMF().mass_mean(), 1)
self.assertAlmostEqual(masses.amin(), 0.10017909529 | units.MSun)
self.assertAlmostEqual(masses.amax(), 19.7132849297 | units.MSun)
def new_cluster(number_of_stars=1000):
masses = new_salpeter_mass_distribution(number_of_stars,
mass_min=0.1 | units.MSun,
mass_max=125.0 | units.MSun,
alpha=-2.35)
nbody_converter = nbody_system.nbody_to_si(masses.sum(), 1 | units.parsec)
particles = new_plummer_model(number_of_stars, nbody_converter)
particles.mass = masses
particles.move_to_center()
return particles
def new_cluster(number_of_stars = 1000):
masses = new_salpeter_mass_distribution(
number_of_stars,
mass_min = 0.1 | units.MSun,
mass_max = 125.0 | units.MSun,
alpha = -2.35
)
nbody_converter = nbody_system.nbody_to_si(masses.sum(), 1 | units.parsec)
particles = new_plummer_model(number_of_stars, nbody_converter)
particles.mass = masses
particles.move_to_center()
return particles
def new_cluster(number_of_stars=1000):
masses = new_salpeter_mass_distribution(number_of_stars,
mass_min=0.1 | units.MSun,
mass_max=125.0 | units.MSun,
alpha=-2.35)
particles = Particles(number_of_stars)
particles.mass = masses
particles.x = units.parsec(random.gamma(2.0, 1.0, number_of_stars))
particles.y = units.parsec(random.gamma(1.0, 1.0, number_of_stars))
particles.z = units.parsec(random.random(number_of_stars))
return particles
def new_cluster(number_of_stars = 1000):
masses = new_salpeter_mass_distribution(
number_of_stars,
mass_min = 0.1 | units.MSun,
mass_max = 125.0 | units.MSun,
alpha = -2.35
)
particles = Particles(number_of_stars)
particles.mass = masses
particles.x = units.parsec(random.gamma(2.0, 1.0, number_of_stars))
particles.y = units.parsec(random.gamma(1.0, 1.0, number_of_stars))
particles.z = units.parsec(random.random(number_of_stars))
return particles
def create_cluster(Ncl, Mstar, Rcl, Mcut):
"""
Create a cluster with Salpeter IMF from 0.1 - Mstar | units.MSun,
distributed in a virialzed Plummer sphere. Split stars into
two particle sets: below_cut and above_cut for m < Mcut; m >= Mcut.
"""
print "Deriving a set of", str(Ncl), "random masses",\
"following a Salpeter IMF between 0.1 and",\
str(Mstar), "MSun (alpha = -2.35)."
salpeter_masses = new_salpeter_mass_distribution(Ncl, mass_max=Mstar)
total_mass = salpeter_masses.sum()
print "Distributing particles in a virialized Plummer sphere."
nbody_converter = nbody_system.nbody_to_si(total_mass, Rcl)
particles = new_plummer_model(Ncl, nbody_converter)
particles.move_to_center()
print "Setting masses of the stars in Plummer sphere."
particles.mass = salpeter_masses
print "Cluster virial radius", particles.virial_radius()
# NB ParticlesSubset does not have the savepoint attribute?!
# Without ,copy(), we have amuse.datamodel.particles.ParticlesSubset
# With .copy(), we have amuse.datamodel.particles.Particles; save works (:
stars_below_cut = particles.select(lambda m: m < Mcut, ["mass"])
stars_above_cut = particles.select(lambda m: m >= Mcut, ["mass"])
print "Number of stars below", str(Mcut), "=", len(stars_below_cut)
print "Number of stars above", str(Mcut), "=", len(stars_above_cut)
try:
import Gnuplot
print "Plotting distribution of stars below and above cut-off."
plotter = Gnuplot.Gnuplot()
plotter('set terminal post enhance color')
plotter('set output "CA_Exam_TLRH_PlummerSphere_SalpeterIMF_splitup.ps"')
plotter.splot(stars_below_cut.position.value_in(units.parsec),
stars_above_cut.position.value_in(units.parsec),)
except ImportError:
print "Unable to produce plot: couldn't find Gnuplot."
except AssertionError:
print "Fails because on of the sets is empty"
# I return the particles superset because the particles superset is saved
# when the subset is changed. This superset can be written to file. (:
return particles, stars_below_cut, stars_above_cut, nbody_converter
def simulate_stellar_evolution(
stellar_evolution=SSE(),
number_of_stars=1000,
end_time=1000.0 | units.Myr,
name_of_the_figure="cluster_HR_diagram.png",
):
"""
A cluster of stars will be created, with masses following a Salpeter IMF.
The stellar evolution will be simulated using any of the legacy codes (SSE,
EVtwin, or MESA).
Finally, a Hertzsprung-Russell diagram will be produced for the final state
of the simulation.
"""
print("The evolution of", str(number_of_stars), "stars will be ",
"simulated until t =", str(end_time), "...")
stellar_evolution.commit_parameters()
print(
"Deriving a set of", str(number_of_stars), "random masses",
"following a Salpeter IMF between 0.1 and 125 MSun (alpha = -2.35).")
salpeter_masses = new_salpeter_mass_distribution(number_of_stars)
print("Initializing the particles")
stars = datamodel.Particles(number_of_stars)
stars.mass = salpeter_masses
print("Stars to evolve:")
print(stars)
stars = stellar_evolution.particles.add_particles(stars)
stellar_evolution.commit_particles()
# print stars.temperature
print("Start evolving...")
stellar_evolution.evolve_model(end_time)
print("Evolved model successfully.")
temperatures = stars.temperature
luminosities = stars.luminosity
stellar_evolution.stop()
plot_HR_diagram(temperatures, luminosities, name_of_the_figure, end_time)
print("All done!")
def simulate_stellar_evolution(
stellar_evolution=SSE(),
number_of_stars=1000,
end_time=1000.0 | units.Myr,
name_of_the_figure="cluster_HR_diagram.png",
):
"""
A cluster of stars will be created, with masses following a Salpeter IMF.
The stellar evolution will be simulated using any of the legacy codes (SSE,
EVtwin, or MESA).
Finally, a Hertzsprung-Russell diagram will be produced for the final state
of the simulation.
"""
print "The evolution of", str(number_of_stars), "stars will be ", \
"simulated until t =", str(end_time), "..."
stellar_evolution.commit_parameters()
print (
"Deriving a set of", str(number_of_stars), "random masses",
"following a Salpeter IMF between 0.1 and 125 MSun (alpha = -2.35).")
salpeter_masses = new_salpeter_mass_distribution(number_of_stars)
print "Initializing the particles"
stars = datamodel.Particles(number_of_stars)
stars.mass = salpeter_masses
print "Stars to evolve:"
print stars
stars = stellar_evolution.particles.add_particles(stars)
stellar_evolution.commit_particles()
# print stars.temperature
print "Start evolving..."
stellar_evolution.evolve_model(end_time)
print "Evolved model successfully."
temperatures = stars.temperature
luminosities = stars.luminosity
stellar_evolution.stop()
plot_HR_diagram(temperatures, luminosities, name_of_the_figure, end_time)
print "All done!"
def populate(self):
if self.repopulate_every_run:
# create nbody_converter thing?
convert_nbody = nbody_system.nbody_to_si(100.0 | units.MSun,
1 | units.parsec)
# instantiate plummer sphere
self.plummer = new_plummer_sphere(self.num_stars, convert_nbody)
self.plummer.x += self.xoffset | units.lightyear
self.plummer.y += self.yoffset | units.lightyear
self.plummer.z += self.zoffset | units.lightyear
# provide mass distribution for stars
self.plummer.mass = new_salpeter_mass_distribution(self.num_stars)
else:
self.plummer = self.initial_plummer
def new_field_stars(
N,
width=10 | units.parsec,
height=10 | units.parsec,
depth=100 | units.parsec,
massdistribution="salpeter",
agespread=3 | units.Gyr,
seed=1701,
):
np.random.seed(seed)
stars = Particles(N)
stars.x = (np.random.random(N) - 0.5) * width
stars.y = (np.random.random(N) - 0.5) * height
stars.z = (np.random.random(N) - 0.02) * depth
if massdistribution == "salpeter":
stars.mass = new_salpeter_mass_distribution(N)
return stars
def demo2(N):
salpeter_masses = new_salpeter_mass_distribution(N)
total_mass = salpeter_masses.sum()
convert_nbody = nbody_system.nbody_to_si(total_mass, 1.0 | units.parsec)
parts = new_plummer_model(N, convert_nbody)
parts.radius = 0. | nbody_system.length
parts.mass = salpeter_masses
parts.move_to_center()
interface = PhiGRAPE(convert_nbody, use_gl=True)
eps = 0.001 | units.parsec
interface.parameters.epsilon_squared = eps**2
interface.particles.add_particles(parts)
return interface
def main():
assert is_mpd_running()
seed = None
nstars = 128
if len(sys.argv) > 1:
stars = int(sys.argv[1])
with_units = len(sys.argv) > 2
if not with_units:
mass_unit = nbody_system.mass
length_unit = nbody_system.length
else:
mass_unit = units.MSun
length_unit = units.parsec
m_min = 0.1 | mass_unit
m_max = 100 | mass_unit
alpha = -2.35
r_vir = 1 | length_unit
masses = new_salpeter_mass_distribution(nstars, m_min, m_max, alpha)
m_tot = masses.sum()
if not with_units:
convert_nbody = None
masses /= m_tot.value_in(nbody_system.mass) # scale to unit mass
m_tot = 1 | nbody_system.mass
else:
convert_nbody = nbody_system.nbody_to_si(m_tot, r_vir)
convert_nbody.set_as_default()
print m_tot
stars = new_plummer_model(nstars, convert_nbody, random_state=seed)
stars.mass = masses
LagrangianRadii(stars, verbose=True)
def generate_cluster(number_of_stars, mass_of_cluster, radius_of_cluster):
# numpy.random.seed(1)
if (mass_of_cluster > 0 | units.MSun):
number_of_stars = int(mass_of_cluster.value_in(units.MSun)) * 5
salpeter_masses = new_salpeter_mass_distribution(number_of_stars)
imf = salpeter_masses
if (mass_of_cluster > 0 | units.MSun):
print("sorted sampling salpeter IMF, total mass:", mass_of_cluster)
imf_cumsum = imf.cumsum()
pick_up_number = (imf_cumsum <= mass_of_cluster).sum()
if (pick_up_number < number_of_stars):
imf_pick_up = imf[:pick_up_number + 1]
sorted_imf_pick_up = np.sort(imf_pick_up)
if (sorted_imf_pick_up[pick_up_number] - mass_of_cluster <
mass_of_cluster - sorted_imf_pick_up[pick_up_number - 1]):
pick_up_number += 1
imf = sorted_imf_pick_up[:pick_up_number]
number_of_stars = pick_up_number
total_mass = imf.sum()
convert_nbody = nbody_system.nbody_to_si(total_mass,
radius_of_cluster | units.parsec)
print("generate plummer model, N=", number_of_stars)
particles = new_plummer_model(number_of_stars, convert_nbody)
print("setting masses of the stars")
particles.radius = 0.0 | units.RSun
particles.mass = imf
#particles.mass[0] = 40.0 |units.MSun
#particles.mass[1] = 50.0 |units.MSun
return particles, convert_nbody
def clustergas(sfeff=0.05,
Nstar=1000,
Ngas=1000,
t_end=30. | units.Myr,
dt_plot=0.05 | units.Myr,
Rscale=0.5 | units.parsec,
runid="runtest",
feedback_efficiency=0.03,
subvirialfac=1.,
grav_code=PhiGRAPE,
gas_code=Gadget2,
se_code=SSEplus,
grav_couple_code=Octgrav,
grav_code_extra=dict(mode='gpu', redirection='none'),
gas_code_extra=dict(number_of_workers=3,
use_gl=False,
redirection='none'),
se_code_extra=dict(redirection='none'),
grav_couple_code_extra=dict()):
try:
os.mkdir(runid)
except:
pass
print "Nstar, Ngas:", Nstar, Ngas
eps = 0.05 * Rscale
eps_star = 0.001 * Rscale
star_masses = new_salpeter_mass_distribution(Nstar,
mass_max=100. | units.MSun)
total_star_mass = star_masses.sum()
total_mass = total_star_mass / sfeff
print "maxmass:", max(star_masses)
print "Tcross", (2.8 *
(Rscale**3 / constants.G / total_star_mass)**0.5).in_(
units.Myr)
print sorted(star_masses)[-10:]
# raise Exception
conv = nbody_system.nbody_to_si(total_mass, Rscale)
star_parts = new_plummer_model(Nstar, convert_nbody=conv)
star_parts.mass = star_masses
star_parts.radius = eps_star
# sub-virialized
star_parts.vx = star_parts.vx * subvirialfac
star_parts.vy = star_parts.vy * subvirialfac
star_parts.vz = star_parts.vz * subvirialfac
print "total cluster mass:", total_mass.in_(units.MSun)
print "star mass:", total_star_mass.in_(units.MSun)
print "gas mass:", (total_mass - total_star_mass).in_(units.MSun)
print "t_end:", conv.to_nbody(t_end)
gas_parts = new_plummer_gas_model(Ngas,
convert_nbody=conv,
base_grid=body_centered_grid_unit_cube)
gas_parts.h_smooth = 0. | units.parsec
gas_parts.mass = gas_parts.mass * (1 - sfeff)
print "gas particle mass:", ((total_mass - total_star_mass) /
len(gas_parts)).in_(units.MSun)
mu = 1.4 | units.amu
gamma1 = 1.6667 - 1
# print 'min Temp:', (gamma1*min(gas_parts.u)*(1.4*units.amu)/constants.kB).in_(units.K)
print 'min Temp:', (gamma1 * min(gas_parts.u) * mu / constants.kB).in_(
units.K)
mgas = (total_mass - total_star_mass) / len(gas_parts)
print max(gas_parts.u)**0.5
dt = smaller_nbody_power_of_two(dt_plot, conv)
dt_star = smaller_nbody_power_of_two(0.001 | units.Myr, conv) #0.001
#original settings
# dt_sph=dt_star
# dt_fast=dt_star*8 # 8
# dt_feedback=dt_fast*2 # 1
#new, improved, more snapshots (thanks inti)
dt_fast = dt / 2 # 8
dt_feedback = dt # 1
feedback_dt = (10. | units.yr, dt_fast)
if not dt_star <= dt_fast <= dt_feedback:
raise Exception
print 'dt_plot:', conv.to_nbody(dt_plot), dt_plot.in_(units.Myr)
print 'dt:', conv.to_nbody(dt), dt.in_(units.Myr)
print 'dt_feedback:', conv.to_nbody(dt_feedback), dt_feedback.in_(
units.Myr)
print 'dt_fast:', conv.to_nbody(dt_fast), dt_fast.in_(units.Myr)
print 'dt_star:', conv.to_nbody(dt_star), dt_star.in_(units.Myr)
star_parts.move_to_center()
gas_parts.move_to_center()
sys = grav_gas_sse(
grav_code,
gas_code,
se_code,
grav_couple_code,
conv,
mgas,
star_parts,
gas_parts,
dt_feedback,
dt_fast,
grav_parameters=(["epsilon_squared",
eps_star**2], ["timestep_parameter", 0.1]),
# ["timestep", dt_star]),
gas_parameters=(
["time_max", 32. | units.Myr],
# ["courant", 0.15 | units.none],
["n_smooth", 64 | units.none],
# ["artificial_viscosity_alpha",1.| units.none],
["n_smooth_tol", 0.005 | units.none],
## NB
["max_size_timestep", dt_fast],
## NB
["time_limit_cpu", 3600000 | units.s]),
couple_parameters=(["epsilon_squared", eps**2], ["opening_angle",
0.5]),
feedback_efficiency=feedback_efficiency,
feedback_radius=0.025 * Rscale,
feedback_dt=feedback_dt,
grav_code_extra=grav_code_extra,
gas_code_extra=gas_code_extra,
se_code_extra=se_code_extra,
grav_couple_code_extra=grav_couple_code_extra)
nsnap = 0
sys.synchronize_model()
t = sys.model_time
tout = t.value_in(units.Myr)
ek = sys.kinetic_energy.value_in(1.e51 * units.erg)
ep = sys.potential_energy.value_in(1.e51 * units.erg)
eth = sys.thermal_energy.value_in(1.e51 * units.erg)
ef = sys.feedback_energy.value_in(1.e51 * units.erg)
print 't Ek Ep Eth Ef:', tout, ek, ep, eth, ef, ek + ep + eth - ef
sys.dump_system_state(runid + "/dump-%6.6i" % nsnap)
print 'max smooth:', max(sys.sph.gas_particles.radius).in_(units.parsec)
print 'mean smooth:', sys.sph.gas_particles.radius.mean().in_(units.parsec)
print 'min smooth:', min(sys.sph.gas_particles.radius).in_(units.parsec)
print 'eps:', eps.in_(units.parsec)
print 'feedback radius:', (0.01 * Rscale).in_(units.parsec)
while (t < t_end - dt / 2):
beginning = time.time()
sys.evolve_model(t + dt)
sys.synchronize_model()
t = sys.model_time
tout = t.value_in(units.Myr)
ek = sys.kinetic_energy.value_in(1.e51 * units.erg)
ep = sys.potential_energy.value_in(1.e51 * units.erg)
eth = sys.thermal_energy.value_in(1.e51 * units.erg)
ef = sys.feedback_energy.value_in(1.e51 * units.erg)
print 't Ek Ep Eth Ef:', tout, ek, ep, eth, ef, ek + ep + eth - ef
nsnap += 1
sys.dump_system_state(runid + "/dump-%6.6i" % nsnap)
end = time.time()
print 'iteration', nsnap, 'took:', (end - beginning), 'seconds'
t_end = o.t_end | units.Myr
dt = o.dt | units.Myr
stellar_evolution = SSE()
stellar_evolution.commit_parameters()
stars = Particles(o.N)
Mmin = o.Mmin | units.MSun
Mmax = o.Mmax | units.MSun
if o.verbose:
print("#Selected parameters: ")
print("#\tN=", o.N)
print("#\tIMF=", o.Mmin, "MSun", o.Mmax, "MSun", o.x_imf)
print("#\t t [Myr] \t <m> [MSun] \t\t d<m>/dt [MSun/Myr]")
stars.mass = new_salpeter_mass_distribution(
o.N, mass_min=Mmin, mass_max=Mmax, alpha=o.x_imf)
stars = stellar_evolution.particles.add_particles(stars)
stellar_evolution.commit_particles()
t = 0 | units.Myr
mm = stars.mass.sum()/len(stars)
while t < t_end:
mm_last = mm
t += dt
stellar_evolution.evolve_model(t)
mm = stars.mass.sum()/len(stars)
dmm_dt = (mm_last-mm)/dt
if o.verbose:
print("t = ", t, "<m>=", mm.as_quantity_in(units.MSun),
" d<m>/dt = ", dmm_dt.as_quantity_in(units.MSun/units.Myr))
else:
def randomparticles_w_ss(N=20, L=1000. | units.AU, dv=2.5 | units.kms):
from amuse.ic.salpeter import new_salpeter_mass_distribution
conv = nbody_system.nbody_to_si(N * 1. | units.MSun, 1000. | units.AU)
conv_sub = nbody_system.nbody_to_si(1. | units.MSun, 50. | units.AU)
dt = smaller_nbody_power_of_two(1000. | units.day, conv)
print(dt.in_(units.day))
dt_param = 0.02
LL = L.value_in(units.AU)
def radius(sys, eta=dt_param, _G=constants.G):
radius = ((_G * sys.total_mass() * dt**2 / eta**2)**(1. / 3.))
# xcm,ycm,zcm=sys.center_of_mass()
# r2max=((sys.x-xcm)**2+(sys.y-ycm)**2+(sys.z-zcm)**2).max()
# if radius < 10 | units.AU:
# radius=20. | units.AU
# return max(radius,r2max**0.5)
return radius * ((len(sys) + 1) / 2.)**0.75
def timestep(ipart, jpart, eta=dt_param / 2, _G=constants.G):
dx = ipart.x - jpart.x
dy = ipart.y - jpart.y
dz = ipart.z - jpart.z
dr2 = dx**2 + dy**2 + dz**2
# if dr2>0:
dr = dr2**0.5
dr3 = dr * dr2
mu = _G * (ipart.mass + jpart.mass)
tau = eta / 2. / 2.**0.5 * (dr3 / mu)**0.5
return tau
numpy.random.seed(7654304)
masses = new_salpeter_mass_distribution(N,
mass_min=0.3 | units.MSun,
mass_max=10. | units.MSun)
#masses=([1.]*10) | units.MSun
stars = Particles(N, mass=masses)
stars.x = L * numpy.random.uniform(-1., 1., N)
stars.y = L * numpy.random.uniform(-1., 1., N)
stars.z = L * 0.
stars.vx = dv * numpy.random.uniform(-1., 1., N)
stars.vy = dv * numpy.random.uniform(-1., 1., N)
stars.vz = dv * 0.
stars.radius = (1. | units.RSun) * (stars.mass /
(1. | units.MSun))**(1. / 3.)
stars.move_to_center()
parts = HierarchicalParticles(stars)
# ss=new_solar_system()[[0,5,6,7,8]]
# parts.assign_subsystem(ss,parts[0])
def parent_worker():
code = Hermite(conv)
code.parameters.epsilon_squared = 0. | units.AU**2
code.parameters.end_time_accuracy_factor = 0.
code.parameters.dt_param = 0.001
print(code.parameters.dt_dia.in_(units.yr))
return code
def sub_worker(parts):
mode = system_type(parts)
if mode == "twobody":
code = TwoBody(conv_sub)
elif mode == "solarsystem":
code = Mercury(conv_sub)
elif mode == "nbody":
code = Huayno(conv_sub)
code.parameters.inttype_parameter = code.inttypes.SHARED4
return code
def py_worker():
code = CalculateFieldForParticles(gravity_constant=constants.G)
return code
nemesis = Nemesis(parent_worker, sub_worker, py_worker)
nemesis.timestep = dt
nemesis.distfunc = timestep
nemesis.threshold = dt
nemesis.radius = radius
nemesis.commit_parameters()
nemesis.particles.add_particles(parts)
nemesis.commit_particles()
tend = 3200. | units.yr
t = 0 | units.yr
dtdiag = dt * 2
time = [0.]
allparts = nemesis.particles.all()
E = allparts.potential_energy() + allparts.kinetic_energy()
E1 = nemesis.potential_energy + nemesis.kinetic_energy
com = allparts.center_of_mass()
mom = allparts.total_momentum()
ang = allparts.total_angular_momentum()
E0 = E
A0 = (ang[0]**2 + ang[1]**2 + ang[2]**2)**0.5
P0 = mom[0].value_in(units.MSun * units.kms)
totalE = [0.]
totalA = [0.]
totalP = [0.]
ss = nemesis.particles.all()
x = (ss.x).value_in(units.AU)
xx = [x]
y = (ss.y).value_in(units.AU)
yy = [y]
nstep = 0
while t < tend - dtdiag / 2:
t += dtdiag
nemesis.evolve_model(t)
print(t.in_(units.yr))
print(len(nemesis.particles))
time.append(t.value_in(units.yr))
allparts = nemesis.particles.all()
E = allparts.potential_energy() + allparts.kinetic_energy()
E1 = nemesis.potential_energy + nemesis.kinetic_energy
ang = allparts.total_angular_momentum()
mom = allparts.total_momentum()
A = (ang[0]**2 + ang[1]**2 + ang[2]**2)**0.5
P = mom[0].value_in(units.MSun * units.kms)
totalE.append(abs((E0 - E) / E0))
totalA.append(abs((A0 - A) / A0))
totalP.append(abs(P0 - P))
print(totalE[-1], (E - E1) / E)
# print allparts.potential_energy(),nemesis.potential_energy
ss = nemesis.particles.all()
x = (ss.x).value_in(units.AU)
y = (ss.y).value_in(units.AU)
lowm = numpy.where(ss.mass.value_in(units.MSun) < 0.1)[0]
highm = numpy.where(ss.mass.value_in(units.MSun) >= 0.1)[0]
xcm = nemesis.particles.x.value_in(units.AU)
ycm = nemesis.particles.y.value_in(units.AU)
r = (nemesis.particles.radius).value_in(units.AU)
xx.append(x)
yy.append(y)
key = ss.key
f = pyplot.figure(figsize=(8, 8))
ax = f.gca()
circles = []
# for i in range(len(xx[0])):
# pyplot.plot(xx[-1][i],yy[-1][i],colors[key[i]%numpy.uint64(len(colors))]+
# markerstyles[key[i]%numpy.uint64(len(markerstyles))],markersize=8,mew=2)
pyplot.plot(xx[-1][highm], yy[-1][highm], 'go', markersize=8, mew=2)
pyplot.plot(xx[-1][lowm], yy[-1][lowm], 'b+', markersize=6, mew=1.5)
for p in nemesis.particles:
# if nemesis.particles.collection_attributes.subsystems.has_key(p):
c = 'k'
ls = 'solid'
code_colors = dict(TwoBody='b',
Mercury='r',
Huayno='g',
Hermite='y')
code_ls = dict(TwoBody='dotted',
Mercury='dashed',
Huayno='dashdot',
Hermite='solid')
if nemesis.subcodes.has_key(p):
c = code_colors[nemesis.subcodes[p].__class__.__name__]
ls = code_ls[nemesis.subcodes[p].__class__.__name__]
x = p.x.value_in(units.AU)
y = p.y.value_in(units.AU)
r = p.radius.value_in(units.AU)
circles.append(
pyplot.Circle((x, y), r, color=c, lw=0.8, ls=ls, fill=False))
for c in circles:
ax.add_artist(c)
# pyplot.plot(xcm,ycm,'k+', markersize=4,mew=1)
pyplot.xlim(-1.2 * LL, 1.2 * LL)
pyplot.ylim(-1.2 * LL, 1.2 * LL)
pyplot.xlabel("AU")
pyplot.text(-580, -580, '%8.2f' % t.value_in(units.yr), fontsize=18)
# pyplot.text(-400,-400,len(nemesis.particles),fontsize=18)
pyplot.savefig('xy%6.6i.png' % nstep, bbox_inches='tight')
f.clear()
pyplot.close(f)
nstep += 1
time = numpy.array(time)
totalE = numpy.array(totalE)
totalA = numpy.array(totalA)
totalP = numpy.array(totalP)
xx = numpy.array(xx)
yy = numpy.array(yy)
f = pyplot.figure(figsize=(8, 8))
pyplot.semilogy(time, totalE, 'r')
pyplot.semilogy(time, totalA, 'g')
pyplot.semilogy(time, totalP, 'b')
pyplot.savefig('dEdA.png')
f = pyplot.figure(figsize=(8, 8))
for i in range(len(xx[0])):
pyplot.plot(xx[:, i], yy[:, i],
colors[i % len(colors)] + linestyles[i % len(linestyles)])
pyplot.xlim(-LL, LL)
pyplot.ylim(-LL, LL)
pyplot.savefig('all-xy.png')
def simulate_small_cluster(number_of_stars,
end_time=40 | units.Myr,
name_of_the_figure="test-2.svg"):
random.seed()
salpeter_masses = new_salpeter_mass_distribution(number_of_stars)
total_mass = salpeter_masses.sum()
convert_nbody = nbody_system.nbody_to_si(total_mass, 1.0 | units.parsec)
convert_nbody.set_as_default()
particles = new_plummer_model(number_of_stars, convert_nbody)
gravity = PhiGRAPE(convert_nbody, mode="gpu")
gravity.initialize_code()
gravity.parameters.timestep_parameter = 0.01
gravity.parameters.initial_timestep_parameter = 0.01
gravity.parameters.epsilon_squared = 0.000001 | units.parsec**2
stellar_evolution = SSE()
stellar_evolution.initialize_module_with_default_parameters()
#print "setting masses of the stars"
particles.radius = 0.0 | units.RSun
#comment out to get plummer masses
particles.mass = salpeter_masses
gravity.particles.add_particles(particles)
gravity.initialize_particles(0.0)
from_model_to_gravity = particles.new_channel_to(gravity.particles)
from_gravity_to_model = gravity.particles.new_channel_to(particles)
time = 0.0 | units.Myr
particles.savepoint(time)
move_particles_to_center_of_mass(particles)
kineticEnergy = gravity.kinetic_energy.value_in(units.J)
potentialEnergy = gravity.potential_energy.value_in(units.J)
ToverV = kineticEnergy / potentialEnergy
file.write(str(time.value_in(units.Myr)))
file.write(' ')
file.write(str(ToverV))
file.write('\n')
while time < end_time:
time += 0.25 | units.Myr
gravity.evolve_model(time)
from_gravity_to_model.copy()
print "Evolved model to t =", str(time)
print "Evolved model to t =", str(
convert_nbody.to_nbody(time.value_in(units.Myr) | units.Myr))
kineticEnergy = gravity.kinetic_energy.value_in(units.J)
potentialEnergy = gravity.potential_energy.value_in(units.J)
ToverV = kineticEnergy / potentialEnergy
print "Kin / Pot =", ToverV
#print "Particle Mass =", particles[1].mass
file.write(str(time.value_in(units.Myr)))
file.write(' ')
file.write(str(ToverV))
file.write('\n')
file.close()
if os.path.exists('small.hdf5'):
os.remove('small.hdf5')
storage = store.StoreHDF("small.hdf5")
storage.store(particles)
del gravity
del stellar_evolution
cluster_populations = []
j = 0 #counter
while j <= Nclusters:
Mcluster = masses[j] | units.MSun
Nstars, Mmin_star, Mmax_star = 100, 0.1, 100.
mZams_flag = 0
while mZams_flag == 0:
mZams = new_salpeter_mass_distribution(Nstars,
Mmin_star | units.MSun,
Mmax_star | units.MSun,
random=np.random)
mass_difference_ratio = (Mcluster - mZams.sum()) / Mcluster
if mass_difference_ratio > 0.01:
Nstars += 1
if mass_difference_ratio < -0.01:
Nstars -= 1
if np.abs(mass_difference_ratio) <= 0.01:
mZams_flag = 1
star_masses = mZams.value_in(units.MSun)
np.savetxt('star_masses_index=%i.txt' % j, star_masses)
stars = int(sys.argv[1])
with_units = len(sys.argv) > 2
if not with_units:
mass_unit = nbody_system.mass
length_unit = nbody_system.length
else:
mass_unit = units.MSun
length_unit = units.parsec
m_min = 0.1 | mass_unit
m_max = 100 | mass_unit
alpha = -2.35
r_vir = 1 | length_unit
masses = new_salpeter_mass_distribution(nstars, m_min, m_max, alpha)
m_tot = masses.sum()
if not with_units:
convert_nbody = None
masses /= m_tot.value_in(nbody_system.mass) # scale to unit mass
m_tot = 1 | nbody_system.mass
else:
convert_nbody = nbody_system.nbody_to_si(m_tot, r_vir)
convert_nbody.set_as_default()
print m_tot
stars = new_plummer_model(nstars, convert_nbody, random_state=seed)
stars.mass = masses
LagrangianRadii(stars, verbose=1)
def simulate_small_cluster(number_of_stars,
end_time=40 | units.Myr,
name_of_the_figure="test-2.svg"):
random.seed()
salpeter_masses = new_salpeter_mass_distribution(number_of_stars)
total_mass = salpeter_masses.sum()
convert_nbody = nbody_system.nbody_to_si(total_mass, 1.0 | units.parsec)
convert_nbody.set_as_default()
print 'end_time:', convert_nbody.to_nbody(end_time)
print convert_nbody.to_nbody(total_mass)
particles = new_plummer_model(number_of_stars, convert_nbody)
gravity = PhiGRAPE(convert_nbody, mode="gpu", use_gl="true")
gravity.parameters.timestep_parameter = 0.01
gravity.parameters.initial_timestep_parameter = 0.01
gravity.parameters.epsilon_squared = 0.0015 | units.parsec**2
particles.radius = 0.0 | units.RSun
# particles.mass = salpeter_masses
move_particles_to_center_of_mass(particles)
gravity.particles.add_particles(particles)
gravity.initialize_particles(0.0)
gravity.start_viewer()
from_model_to_gravity = particles.new_channel_to(gravity.particles)
from_gravity_to_model = gravity.particles.new_channel_to(particles)
time = 0.0 | units.Myr
# particles.savepoint(time)
kineticEnergy = gravity.kinetic_energy.value_in(units.J)
potentialEnergy = gravity.potential_energy.value_in(units.J)
ToverV = kineticEnergy / potentialEnergy
E0 = convert_nbody.to_nbody(gravity.kinetic_energy +
gravity.potential_energy)
file.write(str(time.value_in(units.Myr)))
file.write(' ')
file.write(str(ToverV))
file.write('\n')
gravity.parameters.timestep_parameter = 0.01
gravity.parameters.initial_timestep_parameter = 0.01
while time < end_time:
time += 0.5 * convert_nbody.to_si(1 | nbody_system.time)
gravity.evolve_model(time)
gravity.synchronize_model()
from_gravity_to_model.copy()
print "Evolved model to t =", str(time)
kineticEnergy = gravity.kinetic_energy.value_in(units.J)
potentialEnergy = gravity.potential_energy.value_in(units.J)
ToverV = kineticEnergy / potentialEnergy
Et = convert_nbody.to_nbody(gravity.kinetic_energy +
gravity.potential_energy)
print "Kin / Pot =", ToverV, (Et - E0) / E0
file.write(str(time.value_in(units.Myr)))
file.write(' ')
file.write(str(ToverV))
file.write('\n')
file.close()
if os.path.exists('small.hdf5'):
os.remove('small.hdf5')
storage = store.StoreHDF("small.hdf5")
storage.store(particles)
del gravity
del stellar_evolution
def simulate_small_cluster(number_of_stars,
end_time=40 | units.Myr,
name_of_the_figure="test-2.svg"):
# numpy.random.seed(1)
salpeter_masses = new_salpeter_mass_distribution(number_of_stars)
total_mass = salpeter_masses.sum()
convert_nbody = nbody_system.nbody_to_si(total_mass, 1.0 | units.parsec)
particles = new_plummer_model(number_of_stars, convert_nbody)
gravity = BHTree(convert_nbody)
# print gravity.parameters.timestep.as_quantity_in(units.Myr)
gravity.parameters.timestep = 0.0001 | units.Myr # tiny!
gravity.parameters.epsilon_squared \
= (float(number_of_stars)**(-0.333333) | units.parsec) ** 2
stellar_evolution = SSE()
print "setting masses of the stars"
particles.radius = 0.0 | units.RSun
particles.mass = salpeter_masses
print "initializing the particles"
stellar_evolution.particles.add_particles(particles)
from_stellar_evolution_to_model \
= stellar_evolution.particles.new_channel_to(particles)
from_stellar_evolution_to_model.copy_attributes(["mass"])
print "centering the particles"
particles.move_to_center()
print "scaling particles to viridial equilibrium"
particles.scale_to_standard(convert_nbody)
gravity.particles.add_particles(particles)
from_model_to_gravity = particles.new_channel_to(gravity.particles)
from_gravity_to_model = gravity.particles.new_channel_to(particles)
time = 0.0 | units.Myr
particles.savepoint(time)
total_energy_at_t0 = gravity.kinetic_energy + gravity.potential_energy
print "evolving the model until t = " + str(end_time)
while time < end_time:
time += 0.25 | units.Myr
print "gravity evolve step starting"
gravity.evolve_model(time)
print "gravity evolve step done"
print "stellar evolution step starting"
stellar_evolution.evolve_model(time)
print "stellar evolution step done"
from_gravity_to_model.copy()
from_stellar_evolution_to_model.copy_attributes(["mass", "radius"])
particles.savepoint(time)
from_model_to_gravity.copy_attributes(["mass"])
total_energy_at_this_time \
= gravity.kinetic_energy + gravity.potential_energy
print_log(time, gravity, particles, total_energy_at_t0,
total_energy_at_this_time)
test_results_path = get_path_to_results()
output_file = os.path.join(test_results_path, "small.hdf5")
if os.path.exists(output_file):
os.remove(output_file)
storage = store.StoreHDF(output_file)
storage.store(particles)
gravity.stop()
stellar_evolution.stop()
plot_particles(particles, name_of_the_figure)
def kira(tend, N, R, Nbin):
logging.basicConfig(level=logging.ERROR)
mass = new_salpeter_mass_distribution(N, mass_min=10 | units.MSun)
converter = nbody_system.nbody_to_si(mass.sum(), R)
code = Hermite(converter)
stars = new_plummer_model(N, convert_nbody=converter)
stars.mass = mass
stars.radius = 0.01/len(stars) | R.unit
single_stars, binary_stars, singles_in_binaries \
= make_secondaries(stars, Nbin)
print(binary_stars)
stellar = SeBa()
stellar.particles.add_particles(single_stars)
stellar.particles.add_particles(singles_in_binaries)
stellar.binaries.add_particles(binary_stars)
channel_to_stars = stellar.particles.new_channel_to(stars)
encounter_code = encounters.HandleEncounter(
kepler_code=new_kepler(converter),
resolve_collision_code=new_smalln(converter),
interaction_over_code=None,
G=constants.G
)
multiples_code = encounters.Multiples(
gravity_code=code,
handle_encounter_code=encounter_code,
G=constants.G
)
multiples_code.particles.add_particles((stars-binary_stars).copy())
multiples_code.singles_in_binaries.add_particles(singles_in_binaries)
multiples_code.binaries.add_particles(binary_stars)
multiples_code.commit_particles()
channel_from_stars_to_particles \
= stellar.particles.new_channel_to(multiples_code.particles)
stopping_condition \
= multiples_code.stopping_conditions.binaries_change_detection
stopping_condition.enable()
from matplotlib import pyplot
from distinct_colours import get_distinct
pyplot.rcParams.update({'font.size': 30})
figure = pyplot.figure(figsize=(12, 9))
ax = pyplot.gca()
ax.get_yaxis().get_major_formatter().set_useOffset(False)
ax.xaxis._autolabelpos = True
ax.yaxis._autolabelpos = True
color = get_distinct(2)
pyplot.scatter(numpy.log10(stellar.binaries.semi_major_axis.
value_in(units.AU)),
stellar.binaries.eccentricity, c=color[0], s=200, lw=0)
t = quantities.linspace(0*tend, tend, 11)
for ti in t:
print(("t, Energy=", ti, multiples_code.particles.mass.sum(),
multiples_code.get_total_energy()))
multiples_code.evolve_model(ti)
print(("at t=", multiples_code.model_time,
"Nmultiples:", len(multiples_code.multiples)))
if stopping_condition.is_set():
resolve_changed_binaries(stopping_condition, stellar, converter)
stellar.evolve_model(ti)
channel_from_stars_to_particles.copy_attributes(["mass", "radius"])
update_dynamical_binaries_from_stellar(stellar, multiples_code,
converter)
print(("Lagrangian radii:",
multiples_code.all_singles.LagrangianRadii(converter)))
print(("MC.particles", multiples_code.particles))
print(("Lagrangian radii:",
multiples_code.particles.LagrangianRadii(converter)))
print(("t, Energy=", ti, multiples_code.get_total_energy()))
pyplot.scatter(numpy.log10(stellar.binaries.semi_major_axis
.value_in(units.AU)),
stellar.binaries.eccentricity, c=color[1], lw=0, s=50)
pyplot.xlabel("$\log_{10}(a/R_\odot)$")
pyplot.ylabel("eccentricity")
save_file = 'kira_a_vs_e.pdf'
pyplot.savefig(save_file)
print('\nSaved figure in file', save_file, '\n')
pyplot.show()
stellar.stop()
dt = o.dt | units.Myr
stellar_evolution = SSE()
stellar_evolution.commit_parameters()
stars = Particles(o.N)
Mmin = o.Mmin | units.MSun
Mmax = o.Mmax | units.MSun
if o.verbose:
print("#Selected parameters: ")
print("#\tN=", o.N)
print("#\tIMF=", o.Mmin, "MSun", o.Mmax, "MSun", o.x_imf)
print("#\t t [Myr] \t <m> [MSun] \t\t d<m>/dt [MSun/Myr]")
stars.mass = new_salpeter_mass_distribution(o.N,
mass_min=Mmin,
mass_max=Mmax,
alpha=o.x_imf)
stars = stellar_evolution.particles.add_particles(stars)
stellar_evolution.commit_particles()
t = 0 | units.Myr
mm = stars.mass.sum() / len(stars)
while t < t_end:
mm_last = mm
t += dt
stellar_evolution.evolve_model(t)
mm = stars.mass.sum() / len(stars)
dmm_dt = (mm_last - mm) / dt
if o.verbose:
print("t = ", t, "<m>=", mm.as_quantity_in(units.MSun),
" d<m>/dt = ", dmm_dt.as_quantity_in(units.MSun / units.Myr))
def assignment_2d():
current_cluster_mass = 400 | units.MSun
initial_mass_fraction = 0.84
desired_initial_mass = current_cluster_mass / initial_mass_fraction
masses = new_salpeter_mass_distribution(100000)
mean_salpeter_mass = masses.mean()
print "mean salpeter mass", mean_salpeter_mass
N = int(desired_initial_mass / mean_salpeter_mass)
print "N", N
Rvir = 10 | units.lightyear
z = 0.17
masses = new_salpeter_mass_distribution(N)
converter = nbody_system.nbody_to_si(masses.sum(), Rvir)
G_SI = converter.to_si(nbody_system.G)
bodies = new_plummer_sphere(N, convert_nbody=converter)
bodies.mass = masses
bodies.metalicity = z
# start the gravity solver
gravity = BHTree(converter)
gravity.initialize_code()
gravity.parameters.timestep = 0.1 | units.Myr
# start the stellar evolution solver
stellar = SSE()
stars = stellar.particles.add_particles(bodies)
from_stellar_evolution_to_model \
= stellar.particles.new_channel_to(bodies)
from_stellar_evolution_to_model.copy_attributes(["mass"])
bodies.scale_to_standard(converter)
gravity.particles.add_particles(bodies)
from_model_to_gravity = bodies.new_channel_to(gravity.particles)
from_gravity_to_model = gravity.particles.new_channel_to(bodies)
gravity.commit_particles()
end_time = 1000 | units.Myr
current_time = 0 | units.Myr
cluster = "Hyades"
bound_stars_counts = []
main_sequence_stars_counts = []
giant_stars_counts = []
remnant_stars_counts = []
max_radii = [] | units.parsec
virial_radii = [] | units.parsec
times = [] | units.Myr
while current_time < end_time:
name_of_the_figure = "isochrone_with_grav_"+str(int(current_time.value_in(units.Myr)))+".png"
gravity.evolve_model(current_time)
stellar.evolve_model(current_time)
from_gravity_to_model.copy()
from_stellar_evolution_to_model.copy_attributes(["mass", "radius"])
from_model_to_gravity.copy_attributes(["mass"])
remnant_count = 0
main_sequence_count = 0
giant_count = 0
for star in stars:
if stellar_remnant_state(star):
remnant_count += 1
if stellar_giant_state(star):
giant_count += 1
if stellar_main_sequence_state(star):
main_sequence_count += 1
max_radius = bodies.total_radius()
virial_radius = bodies.virial_radius()
bound_star_count = len(bodies.bound_subset(unit_converter=converter, G=G_SI))
print "bound stars:", bound_star_count
print "main sequence stars:", main_sequence_count
print "giant stars:", giant_count
print "remnant stars:", remnant_count
print "cluster radius(max from centre):", max_radius
print "virial radius:", virial_radius
print current_time
times.append(current_time)
remnant_stars_counts.append(remnant_count)
giant_stars_counts.append(giant_count)
main_sequence_stars_counts.append(main_sequence_count)
max_radii.append(max_radius)
virial_radii.append(virial_radius)
bound_stars_counts.append(bound_star_count)
temperatures = stars.temperature
luminosities = stars.luminosity
plot_HR_diagram(temperatures, luminosities,
cluster+"/",
name_of_the_figure, current_time)
current_time += 10 | units.Myr
data = {}
data["bound_stars_at_time"] = bound_stars_counts
data["remnant_stars_at_time"] = remnant_stars_counts
data["giant_stars_at_time"] = giant_stars_counts
data["main_sequence_stars_at_time"] = main_sequence_stars_counts
data["max_radius_at_time"] = max_radii
data["virial_radii"] = virial_radii
data["times"] = times
pickle.dump(data, open(cluster+"/assignment2d.dat", "wb"))
stars = int(sys.argv[1])
with_units = len(sys.argv) > 2
if not with_units :
mass_unit = nbody_system.mass
length_unit = nbody_system.length
else :
mass_unit = units.MSun
length_unit = units.parsec
m_min = 0.1 | mass_unit
m_max = 100 | mass_unit
alpha = -2.35
r_vir = 1 | length_unit
masses = new_salpeter_mass_distribution(nstars, m_min, m_max, alpha)
m_tot = masses.sum()
if not with_units :
convert_nbody = None
masses /= m_tot.value_in(nbody_system.mass) # scale to unit mass
m_tot = 1 | nbody_system.mass
else :
convert_nbody = nbody_system.nbody_to_si(m_tot, r_vir)
convert_nbody.set_as_default()
print m_tot
stars = new_plummer_model(nstars, convert_nbody, random_state = seed);
stars.mass = masses
LagrangianRadii(stars, verbose=1)
def make_a_star_cluster(
stellar_mass=False,
initial_mass_function="salpeter",
upper_mass_limit=125. | units.MSun,
number_of_stars=1024,
effective_radius=3.0 | units.parsec,
star_distribution="plummer",
star_distribution_w0=7.0,
star_distribution_fd=2.0,
star_metallicity=0.01,
# initial_binary_fraction=0,
**kwargs):
"""
Create stars.
When using an IMF, either the stellar mass is fixed (within
stochastic error) or the number of stars is fixed. When using
equal-mass stars, both are fixed.
"""
if stellar_mass:
# Add stars to cluster, until mass limit reached (inclusive!)
if initial_mass_function == "kroupa":
from amuse.ic.brokenimf import new_kroupa_mass_distribution
mass = new_kroupa_mass_distribution(0)
while mass.sum() < stellar_mass:
mass.append(
new_kroupa_mass_distribution(
1,
mass_max=upper_mass_limit,
)[0])
total_mass = mass.sum()
number_of_stars = len(mass)
elif initial_mass_function == "salpeter":
from amuse.ic.salpeter import new_salpeter_mass_distribution
mass = new_salpeter_mass_distribution(0)
while mass.sum() < stellar_mass:
mass.append(
new_salpeter_mass_distribution(
1,
mass_max=upper_mass_limit,
)[0])
total_mass = mass.sum()
number_of_stars = len(mass)
elif initial_mass_function == "fixed":
mass_of_individual_star = stellar_mass / number_of_stars
mass = mass_of_individual_star
total_mass = stellar_mass
else:
return -1, "No mass function"
else:
# Give stars their mass
if initial_mass_function == "kroupa":
from amuse.ic.brokenimf import new_kroupa_mass_distribution
mass = new_kroupa_mass_distribution(
number_of_stars,
mass_max=upper_mass_limit,
)
total_mass = mass.sum()
elif initial_mass_function == "salpeter":
from amuse.ic.salpeter import new_salpeter_mass_distribution
mass = new_salpeter_mass_distribution(
number_of_stars,
mass_max=upper_mass_limit,
)
total_mass = mass.sum()
elif initial_mass_function == "fixed":
mass = mass_of_individual_star
total_mass = number_of_stars * mass
else:
return -1, "No mass function"
converter = generic_unit_converter.ConvertBetweenGenericAndSiUnits(
total_mass,
1. | units.kms,
effective_radius,
)
# Give stars a position and velocity, based on the distribution model.
if star_distribution == "plummer":
from amuse.ic.plummer import new_plummer_sphere
stars = new_plummer_sphere(
number_of_stars,
convert_nbody=converter,
)
elif star_distribution == "king":
from amuse.ic.kingmodel import new_king_model
stars = new_king_model(
number_of_stars,
star_distribution_w0,
convert_nbody=converter,
)
elif star_distribution == "fractal":
from amuse.ic.fractalcluster import new_fractal_cluster_model
stars = new_fractal_cluster_model(
number_of_stars,
fractal_dimension=star_distribution_fd,
convert_nbody=converter,
)
else:
return -1, "No stellar distribution"
# set the stellar mass.
stars.mass = mass
# set other stellar parameters.
stars.metallicity = star_metallicity
# Virialize the star cluster
stars.move_to_center()
stars.scale_to_standard(
convert_nbody=converter,
# virial_ratio=virial_ratio,
# smoothing_length_squared= ...,
)
# Record the cluster's initial parameters to the particle distribution
stars.collection_attributes.initial_mass_function = initial_mass_function
stars.collection_attributes.upper_mass_limit = upper_mass_limit
stars.collection_attributes.number_of_stars = number_of_stars
stars.collection_attributes.effective_radius = effective_radius
stars.collection_attributes.star_distribution = star_distribution
stars.collection_attributes.star_distribution_w0 = star_distribution_w0
stars.collection_attributes.star_distribution_fd = star_distribution_fd
stars.collection_attributes.star_metallicity = star_metallicity
# Derived/legacy values
stars.collection_attributes.converter_mass = \
converter.to_si(1 | nbody_system.mass)
stars.collection_attributes.converter_length =\
converter.to_si(1 | nbody_system.length)
stars.collection_attributes.converter_speed =\
converter.to_si(1 | nbody_system.speed)
return stars
def simulate_small_cluster(number_of_stars, end_time=40 | units.Myr,
name_of_the_figure="test-2.svg"):
# numpy.random.seed(1)
salpeter_masses = new_salpeter_mass_distribution(number_of_stars)
total_mass = salpeter_masses.sum()
convert_nbody = nbody_system.nbody_to_si(total_mass, 1.0 | units.parsec)
particles = new_plummer_model(number_of_stars, convert_nbody)
gravity = BHTree(convert_nbody)
gravity.initialize_code()
# gravity.parameters.set_defaults()
# print gravity.parameters.timestep.as_quantity_in(units.Myr)
gravity.parameters.timestep = 0.0001 | units.Myr # tiny!
gravity.parameters.epsilon_squared \
= (float(number_of_stars)**(-0.333333) | units.parsec) ** 2
stellar_evolution = SSE()
stellar_evolution.initialize_module_with_default_parameters()
print "setting masses of the stars"
particles.radius = 0.0 | units.RSun
particles.mass = salpeter_masses
print "initializing the particles"
stellar_evolution.particles.add_particles(particles)
from_stellar_evolution_to_model \
= stellar_evolution.particles.new_channel_to(particles)
from_stellar_evolution_to_model.copy_attributes(["mass"])
print "centering the particles"
particles.move_to_center()
print "scaling particles to viridial equilibrium"
particles.scale_to_standard(convert_nbody)
gravity.particles.add_particles(particles)
from_model_to_gravity = particles.new_channel_to(gravity.particles)
from_gravity_to_model = gravity.particles.new_channel_to(particles)
gravity.commit_particles()
time = 0.0 | units.Myr
particles.savepoint(time)
total_energy_at_t0 = gravity.kinetic_energy + gravity.potential_energy
print "evolving the model until t = " + str(end_time)
while time < end_time:
time += 0.25 | units.Myr
print "Gravity evolve step starting"
gravity_evolve = gravity.evolve_model.async(time)
print "Stellar evolution step starting"
stellar_evolution_evolve = stellar_evolution.evolve_model(time)
print "Stellar evolution step done."
gravity_evolve.result()
print "Gravity evolve step done."
from_gravity_to_model.copy()
from_stellar_evolution_to_model.copy_attributes(["mass", "radius"])
particles.savepoint(time)
from_model_to_gravity.copy_attributes(["mass"])
total_energy_at_this_time \
= gravity.kinetic_energy + gravity.potential_energy
print_log(time, gravity, particles,
total_energy_at_t0, total_energy_at_this_time)
test_results_path = get_path_to_results()
output_file = os.path.join(test_results_path, "small.hdf5")
if os.path.exists(output_file):
os.remove(output_file)
storage = store.StoreHDF(output_file)
storage.store(particles)
gravity.stop()
stellar_evolution.stop()
plot_particles(particles, name_of_the_figure)
def create_cluster_isochrone(cluster, algorithm=SSE,
number_of_stars=1339,
end_time=1000 | units.Myr,
z=0.012
):
"""
Code for Assignment 2B.
@param cluster: Name of cluter (used as dir to store data)
@param stellar: specify the stellar evolution code.
valid options are:
MESA, EVtwin (both Henyey)
SSE, SeBa (both parameterized)
@param number_of_stars: how many stars to evolve
@param end_time: how long the cluster is evolved
@return: dumps the data to file
"""
data = {}
stellar = algorithm()
algorithm_name = str(algorithm).split('.')[-1][:-2]
print "Deriving a set of {0} random masses ".format(number_of_stars),
print "following a Salpeter IMF between 0.1 and 125 Msun",
print "(alpha = -2.35)."
salpeter_masses = new_salpeter_mass_distribution(number_of_stars)
print "Initializing the particles"
stars = datamodel.Particles(number_of_stars)
stars.mass = salpeter_masses
total_mass = 0 | units.MSun
for m in stars.mass: total_mass += m
print "total mass =", total_mass
data['initial_total_mass'] = total_mass
stars.metallicity = z
print "The evolution of {0} stars will be".format(number_of_stars),
print "simulated until t = {0}".format(end_time),
print ", using algorithm {0}".format(algorithm_name)
stellar.commit_parameters()
print "Stars to evolve:"
print stars
data['stars'] = stars
stars = stellar.particles.add_particles(stars)
stellar.commit_particles()
print "Start evolving..."
# stellar.evolve_model(end_time)
times = [] | units.Myr
luminosity_at_time = [] | units.LSun
temperatures_at_time = [] | units.K
mass_at_time = [] | units.MSun
current_time = 0 | units.Myr
while current_time < end_time:
name_of_the_figure = "isochrone_{0}_{1}_{2}.png".\
format(algorithm_name, number_of_stars,
int(current_time.value_in(units.Myr)))
stellar.evolve_model(current_time)
temperatures = stars.temperature
luminosities = stars.luminosity
times.append(current_time)
luminosity_at_time.append(luminosities)
temperatures_at_time.append(temperatures)
mass_at_time.append(stars.total_mass())
print current_time
plot_HR_diagram(temperatures, luminosities,
cluster+"/",
name_of_the_figure, current_time)
current_time += 10 | units.Myr
print "Evolved model successfully."
stellar.stop()
print "All done!"
data['times'] = times
data['luminosity_at_time'] = luminosity_at_time
data['temperatures_at_time'] = temperatures_at_time
data['mass_at_time'] = mass_at_time
print data
pickle.dump(data, open(cluster+"/assignment2b.dat", "wb"))
