def get_galaxies_in_orbit(m_a=10.e11|units.MSun,
m_b=10.e11|units.MSun,
ecc=0.5,
r_min=25.|units.kpc,
t_start=None):
"""
binary galaxy with orbit of given parameters
-- if ecc=>1, start at t_start (p625, t_start=-10=-10*100Myr)
-- if ecc<1, start at apocenter (p644)
"""
converter=nbody_system.nbody_to_si(m_a+m_b,1|units.kpc)
semi = r_min/(1.-ecc)
# relative position and velocity vectors at the pericenter using kepler
kepler = Kepler_twobody(converter)
kepler.initialize_code()
kepler.initialize_from_elements(mass=(m_a+m_b), semi=semi, ecc=ecc, periastron=r_min) # at periastron
# evolve back till initial position
if ( ecc<1. ):
kepler.return_to_apastron()
else:
kepler.transform_to_time(t_start)
# get time of the orbit
t_orbit = kepler.get_time()
rl = kepler.get_separation_vector()
r = [rl[0].value_in(units.AU), rl[1].value_in(units.AU), rl[2].value_in(units.AU)] | units.AU
vl = kepler.get_velocity_vector()
v = [vl[0].value_in(units.kms), vl[1].value_in(units.kms), vl[2].value_in(units.kms)] | units.kms
kepler.stop()
# assign particle atributes
galaxies = Particles(2)
galaxies[0].mass = m_a
galaxies[0].position = (0,0,0) | units.AU
galaxies[0].velocity = (0,0,0) | units.kms
galaxies[1].mass = m_b
galaxies[1].position = r
galaxies[1].velocity = v
# identification
galaxies[0].id = 'a0'
galaxies[1].id = 'b0'
galaxies.move_to_center()
return galaxies, t_orbit
def relative_position_and_velocity_from_orbital_elements(
mass1, mass2, semimajor_axis, eccentricity, mean_anomaly, seed=None):
"""
Function that returns relative positions and velocity vectors or orbiters with masses
mass2 of the central body with mass mass1 in Cartesian coordinates;
for vectors of orbital elements -- semi-major axes, eccentricities, mean anomalies.
3D orientation of orbits (inclination, longitude of ascending node and argument of periapsis) are random.
(cos(incl) is uniform -1--1, longitude of ascending node and argument of periapsis are uniform 0--2pi)
Assuming mass1 is static in the center [0,0,0] m, [0,0,0] km/s (that is mass2<<mass1)
"""
position_vectors = []
velocity_vectors = []
converter = nbody_system.nbody_to_si(1 | units.MSun, 1 | units.AU)
kepler = Kepler(converter)
kepler.initialize_code()
r_vec = (0., 0., 0.) | units.AU
v_vec = (0., 0., 0.) | units.kms
# to change seed for each particle
if seed is not None:
i = 0
for m2_i, a_i, ecc_i, ma_i in zip(mass2, semimajor_axis, eccentricity,
mean_anomaly):
#print m2_i, a_i, ecc_i, ma_i
if seed is not None:
kepler.set_random(seed + i)
i = i + 1
kepler.initialize_from_elements(mass=(mass1 + m2_i),
semi=a_i,
ecc=ecc_i,
mean_anomaly=ma_i,
random_orientation=-1)
ri = kepler.get_separation_vector()
vi = kepler.get_velocity_vector()
# this is to get ~half of the orbits retrograde (that is with inclination
# of 90--180 degrees) --> velocity = -velocity
vel_vec_dir = numpy.random.random()
if (vel_vec_dir <= 0.5):
vel_orientation = 1.
else:
vel_orientation = -1.
position_vectors.append([ri[0], ri[1], ri[2]])
velocity_vectors.append([
vel_orientation * vi[0], vel_orientation * vi[1],
vel_orientation * vi[2]
])
kepler.stop()
return position_vectors, velocity_vectors
def relative_position_and_velocity_from_orbital_elements(mass1,
mass2,
semimajor_axis,
eccentricity,
mean_anomaly,
seed=None):
"""
Function that returns relative positions and velocity vectors or orbiters with masses
mass2 of the central body with mass mass1 in Cartesian coordinates;
for vectors of orbital elements -- semi-major axes, eccentricities, mean anomalies.
3D orientation of orbits (inclination, longitude of ascending node and argument of periapsis) are random.
(cos(incl) is uniform -1--1, longitude of ascending node and argument of periapsis are uniform 0--2pi)
Assuming mass1 is static in the center [0,0,0] m, [0,0,0] km/s (that is mass2<<mass1)
"""
position_vectors = []
velocity_vectors = []
converter = nbody_system.nbody_to_si(1|units.MSun,1|units.AU)
kepler = Kepler(converter)
kepler.initialize_code()
r_vec = (0.,0.,0.) | units.AU
v_vec = (0.,0.,0.) | units.kms
# to change seed for each particle
if seed is not None:
i=0
for m2_i, a_i, ecc_i, ma_i in zip(mass2, semimajor_axis, eccentricity, mean_anomaly):
#print m2_i, a_i, ecc_i, ma_i
if seed is not None:
kepler.set_random(seed+i)
i=i+1
kepler.initialize_from_elements(mass=(mass1+m2_i),semi=a_i,ecc=ecc_i,mean_anomaly=ma_i,random_orientation=-1)
ri = kepler.get_separation_vector()
vi = kepler.get_velocity_vector()
# this is to get ~half of the orbits retrograde (that is with inclination
# of 90--180 degrees) --> velocity = -velocity
vel_vec_dir = numpy.random.random()
if (vel_vec_dir<=0.5):
vel_orientation = 1.
else:
vel_orientation = -1.
position_vectors.append([ri[0], ri[1], ri[2]])
velocity_vectors.append([vel_orientation*vi[0], vel_orientation*vi[1], vel_orientation*vi[2]])
kepler.stop()
return position_vectors, velocity_vectors
def run_kepler(mass, semi, ecc, time):
kep = Kepler(redirection='none')
kep.initialize_code()
kep.set_longitudinal_unit_vector(1.0, 1.0,
0.0)
kep.initialize_from_elements(mass, semi, ecc)
a,e = kep.get_elements()
p = kep.get_periastron()
print "elements:", a, e, p
kep.transform_to_time(time)
x,y,z = kep.get_separation_vector()
print "separation:", x,y,z
x,y,z = kep.get_longitudinal_unit_vector()
print "longitudinal:", x,y,z
pos = [1, 0, 0] | nbody_system.length
vel = [0, 0.5, 0] | nbody_system.speed
kep.initialize_from_dyn(mass, pos[0], pos[1], pos[2],
vel[0], vel[1], vel[2])
a,e = kep.get_elements()
p = kep.get_periastron()
print "elements:", a, e, p
kep.transform_to_time(time)
x,y,z = kep.get_separation_vector()
print "separation:", x,y,z
x,y,z = kep.get_velocity_vector()
print "velocity:", x,y,z
x,y,z = kep.get_longitudinal_unit_vector()
print "longitudinal:", x,y,z
kep.set_random(42)
kep.make_binary_scattering(0.5 | nbody_system.mass,
0.5,
0.5 | nbody_system.mass,
0.0 | nbody_system.speed,
0.0 | nbody_system.length,
1.e-6,
0)
kep.stop()
def test11(self):
"""
testing orbital_elements_for_rel_posvel_arrays for unbound orbits
"""
from amuse.community.kepler.interface import Kepler
numpy.random.seed(66)
N = 10
mass_sun = 1. | units.MSun
mass1 = numpy.ones(N) * mass_sun
mass2 = numpy.zeros(N) | units.MSun
semi_major_axis=-1000.*(random.random(N)) | units.AU
eccentricity = (1.+random.random(N))*10.-9.
inclination = numpy.pi*random.random(N)
longitude_of_the_ascending_node = 2.*numpy.pi*random.random(N)-numpy.pi
argument_of_periapsis = 2.*numpy.pi*random.random(N)-numpy.pi
# kepler.initialize_from_elements initializes orbits with mean_anomaly=0 and true_anomaly=0
true_anomaly = 0.*(360.*random.random(N)-180.)
comets = datamodel.Particles(N)
converter = nbody_system.nbody_to_si(1|units.MSun,1|units.AU)
kepler = Kepler(converter)
kepler.initialize_code()
for i,arg in enumerate(zip(mass1,mass2,semi_major_axis,eccentricity,true_anomaly,inclination,
longitude_of_the_ascending_node,argument_of_periapsis)):
kepler.initialize_from_elements(mass=(mass1[i]+mass2[i]),
semi=semi_major_axis[i],
ecc=eccentricity[i])
ri = kepler.get_separation_vector()
vi = kepler.get_velocity_vector()
om = longitude_of_the_ascending_node[i]
w = argument_of_periapsis[i]
incl = inclination[i]
a1 = ([numpy.cos(om), -numpy.sin(om), 0.0], [numpy.sin(om), numpy.cos(om), 0.0], [0.0, 0.0, 1.0])
a2 = ([1.0, 0.0, 0.0], [0.0, numpy.cos(incl), -numpy.sin(incl)], [0.0, numpy.sin(incl), numpy.cos(incl)])
a3 = ([numpy.cos(w), -numpy.sin(w), 0.0], [numpy.sin(w), numpy.cos(w), 0.0], [0.0, 0.0, 1.0])
A = numpy.dot(numpy.dot(a1,a2),a3)
r_vec = numpy.dot(A,numpy.reshape(ri,3,1))
v_vec = numpy.dot(A,numpy.reshape(vi,3,1))
r = (0.0, 0.0, 0.0) | units.AU
v = (0.0, 0.0, 0.0) | (units.AU / units.day)
r[0] = r_vec[0]
r[1] = r_vec[1]
r[2] = r_vec[2]
v[0] = v_vec[0]
v[1] = v_vec[1]
v[2] = v_vec[2]
comets[i].mass = mass2[i]
comets[i].position = r_vec
comets[i].velocity = v_vec
kepler.stop()
semi_major_axis_ext, eccentricity_ext, ta_ext, inclination_ext, \
longitude_of_the_ascending_node_ext, argument_of_periapsis_ext = \
orbital_elements(comets.position,
comets.velocity,
comets.mass + mass_sun,
G=constants.G)
self.assertAlmostEqual(semi_major_axis,semi_major_axis_ext.in_(units.AU))
self.assertAlmostEqual(eccentricity,eccentricity_ext)
self.assertAlmostEqual(inclination,inclination_ext)
self.assertAlmostEqual(longitude_of_the_ascending_node,longitude_of_the_ascending_node_ext)
self.assertAlmostEqual(argument_of_periapsis,argument_of_periapsis_ext)
self.assertAlmostEqual(true_anomaly,ta_ext)
def run_ph4(infile = None, outfile = None,
number_of_stars = 100, number_of_binaries = 0,
end_time = 10 | nbody_system.time,
delta_t = 1 | nbody_system.time,
n_workers = 1, use_gpu = 1, gpu_worker = 1,
salpeter = 0,
accuracy_parameter = 0.1,
softening_length = 0.0 | nbody_system.length,
manage_encounters = 1, random_seed = 1234):
if random_seed <= 0:
numpy.random.seed()
random_seed = numpy.random.randint(1, pow(2,31)-1)
numpy.random.seed(random_seed)
print "random seed =", random_seed
if infile != None: print "input file =", infile
print "end_time =", end_time.number
print "delta_t =", delta_t.number
print "n_workers =", n_workers
print "use_gpu =", use_gpu
print "manage_encounters =", manage_encounters
print "\ninitializing the gravity module"
sys.stdout.flush()
init_smalln()
# Note that there are actually three GPU options:
#
# 1. use the GPU code and allow GPU use (default)
# 2. use the GPU code but disable GPU use (-g)
# 3. use the non-GPU code (-G)
if gpu_worker == 1:
try:
gravity = grav(number_of_workers = n_workers,
redirection = "none", mode = "gpu")
except Exception as ex:
gravity = grav(number_of_workers = n_workers,
redirection = "none")
else:
gravity = grav(number_of_workers = n_workers,
redirection = "none")
gravity.initialize_code()
gravity.parameters.set_defaults()
#-----------------------------------------------------------------
if infile == None:
print "making a Plummer model"
stars = new_plummer_model(number_of_stars)
id = numpy.arange(number_of_stars)
stars.id = id+1
print "setting particle masses and radii"
if salpeter == 0:
print 'equal masses'
total_mass = 1.0 | nbody_system.mass
scaled_mass = total_mass / number_of_stars
else:
print 'salpeter mass function'
scaled_mass = new_salpeter_mass_distribution_nbody(number_of_stars)
stars.mass = scaled_mass
print "centering stars"
stars.move_to_center()
print "scaling stars to virial equilibrium"
stars.scale_to_standard(smoothing_length_squared
= gravity.parameters.epsilon_squared)
else:
# Read the input data. Units are dynamical (sorry).
# Format: id mass pos[3] vel[3]
print "reading file", infile
id = []
mass = []
pos = []
vel = []
f = open(infile, 'r')
count = 0
for line in f:
if len(line) > 0:
count += 1
cols = line.split()
if count == 1: snap = int(cols[0])
elif count == 2: number_of_stars = int(cols[0])
elif count == 3: time = float(cols[0]) | nbody_system.time
else:
if len(cols) >= 8:
id.append(int(cols[0]))
mass.append(float(cols[1]))
pos.append((float(cols[2]),
float(cols[3]), float(cols[4])))
vel.append((float(cols[5]),
float(cols[6]), float(cols[7])))
f.close()
stars = datamodel.Particles(number_of_stars)
stars.id = id
stars.mass = mass | nbody_system.mass
stars.position = pos | nbody_system.length
stars.velocity = vel | nbody_system.speed
#stars.radius = 0. | nbody_system.length
total_mass = stars.mass.sum()
ke = pa.kinetic_energy(stars)
kT = ke/(1.5*number_of_stars)
if number_of_binaries > 0:
# Turn selected stars into binary components.
# Only tested for equal-mass case.
kep = Kepler(redirection = "none")
kep.initialize_code()
added_mass = 0.0 | nbody_system.mass
# Work with energies rather than semimajor axes.
Emin = 10*kT
Emax = 20*kT
ecc = 0.1
id_count = number_of_stars
nbin = 0
for i in range(0, number_of_stars,
number_of_stars/number_of_binaries):
# Star i is CM, becomes component, add other star at end.
nbin += 1
mass = stars[i].mass
new_mass = numpy.random.uniform()*mass # uniform q?
mbin = mass + new_mass
fac = new_mass/mbin
E = Emin + numpy.random.uniform()*(Emax-Emin)
a = 0.5*nbody_system.G*mass*new_mass/E
kep.initialize_from_elements(mbin, a, ecc)
dr = quantities.AdaptingVectorQuantity()
dr.extend(kep.get_separation_vector())
dv = quantities.AdaptingVectorQuantity()
dv.extend(kep.get_velocity_vector())
newstar = datamodel.Particles(1)
newstar.mass = new_mass
newstar.position = stars[i].position + (1-fac)*dr
newstar.velocity = stars[i].velocity + (1-fac)*dv
# stars[i].mass = mass
stars[i].position = stars[i].position - fac*dr
stars[i].velocity = stars[i].velocity - fac*dv
id_count += 1
newstar.id = id_count
stars.add_particles(newstar)
added_mass += new_mass
if nbin >= number_of_binaries: break
kep.stop()
print 'created', nbin, 'binaries'
sys.stdout.flush()
stars.mass = stars.mass * total_mass/(total_mass+added_mass)
number_of_stars += nbin
# Set dynamical radii (assuming virial equilibrium and standard
# units). Note that this choice should be refined, and updated
# as the system evolves. Probably the choice of radius should be
# made entirely in the multiples module. TODO. In these units,
# M = 1 and <v^2> = 0.5, so the mean 90-degree turnaround impact
# parameter is
#
# b_90 = G (m_1+m_2) / vrel^2
# = 2 <m> / 2<v^2>
# = 2 / N for equal masses
#
# Taking r_i = m_i / 2<v^2> = m_i in virial equilibrium means
# that, approximately, "contact" means a 90-degree deflection (r_1
# + r_2 = b_90). A more conservative choice with r_i less than
# this value will isolates encounters better, but also place more
# load on the large-N dynamical module.
stars.radius = stars.mass.number | nbody_system.length
time = 0.0 | nbody_system.time
# print "IDs:", stars.id.number
print "recentering stars"
stars.move_to_center()
sys.stdout.flush()
#-----------------------------------------------------------------
if softening_length < 0.0 | nbody_system.length:
# Use ~interparticle spacing. Assuming standard units here. TODO
eps2 = 0.25*(float(number_of_stars))**(-0.666667) \
| nbody_system.length**2
else:
eps2 = softening_length*softening_length
print 'softening length =', eps2.sqrt()
gravity.parameters.timestep_parameter = accuracy_parameter
gravity.parameters.epsilon_squared = eps2
gravity.parameters.use_gpu = use_gpu
# gravity.parameters.manage_encounters = manage_encounters
print ''
print "adding particles"
# print stars
sys.stdout.flush()
gravity.particles.add_particles(stars)
gravity.commit_particles()
print ''
print "number_of_stars =", number_of_stars
print "evolving to time =", end_time.number, \
"in steps of", delta_t.number
sys.stdout.flush()
# Channel to copy values from the code to the set in memory.
channel = gravity.particles.new_channel_to(stars)
stopping_condition = gravity.stopping_conditions.collision_detection
stopping_condition.enable()
# Debugging: prevent the multiples code from being called.
if 0:
stopping_condition.disable()
print 'stopping condition disabled'
sys.stdout.flush()
# -----------------------------------------------------------------
# Create the coupled code and integrate the system to the desired
# time, managing interactions internally.
kep = init_kepler(stars[0], stars[1])
multiples_code = multiples.Multiples(gravity, new_smalln, kep)
multiples_code.neighbor_perturbation_limit = 0.1
#multiples_code.neighbor_distance_factor = 1.0
#multiples_code.neighbor_veto = False
#multiples_code.neighbor_distance_factor = 2.0
multiples_code.neighbor_veto = True
print ''
print 'multiples_code.initial_scale_factor =', \
multiples_code.initial_scale_factor
print 'multiples_code.neighbor_perturbation_limit =', \
multiples_code.neighbor_perturbation_limit
print 'multiples_code.neighbor_veto =', \
multiples_code.neighbor_veto
print 'multiples_code.final_scale_factor =', \
multiples_code.final_scale_factor
print 'multiples_code.initial_scatter_factor =', \
multiples_code.initial_scatter_factor
print 'multiples_code.final_scatter_factor =', \
multiples_code.final_scatter_factor
print 'multiples_code.retain_binary_apocenter =', \
multiples_code.retain_binary_apocenter
print 'multiples_code.wide_perturbation_limit =', \
multiples_code.wide_perturbation_limit
pre = "%%% "
E0,cpu0 = print_log(pre, time, multiples_code)
while time < end_time:
time += delta_t
multiples_code.evolve_model(time)
# Copy values from the module to the set in memory.
channel.copy()
# Copy the index (ID) as used in the module to the id field in
# memory. The index is not copied by default, as different
# codes may have different indices for the same particle and
# we don't want to overwrite silently.
channel.copy_attribute("index_in_code", "id")
print_log(pre, time, multiples_code, E0, cpu0)
sys.stdout.flush()
#-----------------------------------------------------------------
if not outfile == None:
# Write data to a file.
f = open(outfile, 'w')
#--------------------------------------------------
# Need to save top-level stellar data and parameters.
# Need to save multiple data and parameters.
f.write('%.15g\n'%(time.number))
for s in multiples_code.stars: write_star(s, f)
#--------------------------------------------------
f.close()
print 'wrote file', outfile
print ''
gravity.stop()
def run_ph4(infile = None, outfile = None,
number_of_stars = 100, number_of_binaries = 0,
end_time = 10 | nbody_system.time,
delta_t = 1 | nbody_system.time,
n_workers = 1, use_gpu = 1, gpu_worker = 1,
salpeter = 0,
accuracy_parameter = 0.1,
softening_length = 0.0 | nbody_system.length,
manage_encounters = 1, random_seed = 1234):
if random_seed <= 0:
numpy.random.seed()
random_seed = numpy.random.randint(1, pow(2,31)-1)
numpy.random.seed(random_seed)
print "random seed =", random_seed
if infile != None: print "input file =", infile
print "end_time =", end_time.number
print "delta_t =", delta_t.number
print "n_workers =", n_workers
print "use_gpu =", use_gpu
print "manage_encounters =", manage_encounters
print "\ninitializing the gravity module"
sys.stdout.flush()
init_smalln()
# Note that there are actually three GPU options:
#
# 1. use the GPU code and allow GPU use (default)
# 2. use the GPU code but disable GPU use (-g)
# 3. use the non-GPU code (-G)
if gpu_worker == 1:
try:
gravity = grav(number_of_workers = n_workers,
redirection = "none", mode = "gpu")
except Exception as ex:
gravity = grav(number_of_workers = n_workers,
redirection = "none")
else:
gravity = grav(number_of_workers = n_workers,
redirection = "none")
gravity.initialize_code()
gravity.parameters.set_defaults()
#-----------------------------------------------------------------
if infile == None:
print "making a Plummer model"
stars = new_plummer_model(number_of_stars)
id = numpy.arange(number_of_stars)
stars.id = id+1
print "setting particle masses and radii"
if salpeter == 0:
print 'equal masses'
total_mass = 1.0 | nbody_system.mass
scaled_mass = total_mass / number_of_stars
else:
print 'salpeter mass function'
scaled_mass = new_salpeter_mass_distribution_nbody(number_of_stars)
stars.mass = scaled_mass
print "centering stars"
stars.move_to_center()
print "scaling stars to virial equilibrium"
stars.scale_to_standard(smoothing_length_squared
= gravity.parameters.epsilon_squared)
else:
# Read the input data. Units are dynamical (sorry).
# Format: id mass pos[3] vel[3]
print "reading file", infile
id = []
mass = []
pos = []
vel = []
f = open(infile, 'r')
count = 0
for line in f:
if len(line) > 0:
count += 1
cols = line.split()
if count == 1: snap = int(cols[0])
elif count == 2: number_of_stars = int(cols[0])
elif count == 3: time = float(cols[0]) | nbody_system.time
else:
if len(cols) >= 8:
id.append(int(cols[0]))
mass.append(float(cols[1]))
pos.append((float(cols[2]),
float(cols[3]), float(cols[4])))
vel.append((float(cols[5]),
float(cols[6]), float(cols[7])))
f.close()
stars = datamodel.Particles(number_of_stars)
stars.id = id
stars.mass = mass | nbody_system.mass
stars.position = pos | nbody_system.length
stars.velocity = vel | nbody_system.speed
#stars.radius = 0. | nbody_system.length
total_mass = stars.mass.sum()
ke = pa.kinetic_energy(stars)
kT = ke/(1.5*number_of_stars)
if number_of_binaries > 0:
# Turn selected stars into binary components.
# Only tested for equal-mass case.
kep = Kepler(redirection = "none")
kep.initialize_code()
added_mass = 0.0 | nbody_system.mass
# Work with energies rather than semimajor axes.
Emin = 10*kT
Emax = 20*kT
ecc = 0.1
id_count = number_of_stars
nbin = 0
for i in range(0, number_of_stars,
number_of_stars/number_of_binaries):
# Star i is CM, becomes component, add other star at end.
nbin += 1
mass = stars[i].mass
new_mass = numpy.random.uniform()*mass # uniform q?
mbin = mass + new_mass
fac = new_mass/mbin
E = Emin + numpy.random.uniform()*(Emax-Emin)
a = 0.5*nbody_system.G*mass*new_mass/E
kep.initialize_from_elements(mbin, a, ecc)
dr = quantities.AdaptingVectorQuantity()
dr.extend(kep.get_separation_vector())
dv = quantities.AdaptingVectorQuantity()
dv.extend(kep.get_velocity_vector())
newstar = datamodel.Particles(1)
newstar.mass = new_mass
newstar.position = stars[i].position + (1-fac)*dr
newstar.velocity = stars[i].velocity + (1-fac)*dv
# stars[i].mass = mass
stars[i].position = stars[i].position - fac*dr
stars[i].velocity = stars[i].velocity - fac*dv
id_count += 1
newstar.id = id_count
stars.add_particles(newstar)
added_mass += new_mass
if nbin >= number_of_binaries: break
kep.stop()
print 'created', nbin, 'binaries'
sys.stdout.flush()
stars.mass = stars.mass * total_mass/(total_mass+added_mass)
number_of_stars += nbin
# Set dynamical radii (assuming virial equilibrium and standard
# units). Note that this choice should be refined, and updated
# as the system evolves. Probably the choice of radius should be
# made entirely in the multiples module. TODO. In these units,
# M = 1 and <v^2> = 0.5, so the mean 90-degree turnaround impact
# parameter is
#
# b_90 = G (m_1+m_2) / vrel^2
# = 2 <m> / 2<v^2>
# = 2 / N for equal masses
#
# Taking r_i = m_i / 2<v^2> = m_i in virial equilibrium means
# that, approximately, "contact" means a 90-degree deflection (r_1
# + r_2 = b_90). A more conservative choice with r_i less than
# this value will isolates encounters better, but also place more
# load on the large-N dynamical module.
stars.radius = stars.mass.number | nbody_system.length
time = 0.0 | nbody_system.time
# print "IDs:", stars.id.number
print "recentering stars"
stars.move_to_center()
sys.stdout.flush()
#-----------------------------------------------------------------
if softening_length < 0.0 | nbody_system.length:
# Use ~interparticle spacing. Assuming standard units here. TODO
eps2 = 0.25*(float(number_of_stars))**(-0.666667) \
| nbody_system.length**2
else:
eps2 = softening_length*softening_length
print 'softening length =', eps2.sqrt()
gravity.parameters.timestep_parameter = accuracy_parameter
gravity.parameters.epsilon_squared = eps2
gravity.parameters.use_gpu = use_gpu
# gravity.parameters.manage_encounters = manage_encounters
print ''
print "adding particles"
# print stars
sys.stdout.flush()
gravity.particles.add_particles(stars)
gravity.commit_particles()
print ''
print "number_of_stars =", number_of_stars
print "evolving to time =", end_time.number, \
"in steps of", delta_t.number
sys.stdout.flush()
# Channel to copy values from the code to the set in memory.
channel = gravity.particles.new_channel_to(stars)
stopping_condition = gravity.stopping_conditions.collision_detection
stopping_condition.enable()
# Debugging: prevent the multiples code from being called.
if 0:
stopping_condition.disable()
print 'stopping condition disabled'
sys.stdout.flush()
# -----------------------------------------------------------------
# Create the coupled code and integrate the system to the desired
# time, managing interactions internally.
kep = init_kepler(stars[0], stars[1])
multiples_code = multiples.Multiples(gravity, new_smalln, kep)
multiples_code.neighbor_perturbation_limit = 0.1
#multiples_code.neighbor_distance_factor = 1.0
#multiples_code.neighbor_veto = False
#multiples_code.neighbor_distance_factor = 2.0
multiples_code.neighbor_veto = True
print ''
print 'multiples_code.initial_scale_factor =', \
multiples_code.initial_scale_factor
print 'multiples_code.neighbor_perturbation_limit =', \
multiples_code.neighbor_perturbation_limit
print 'multiples_code.neighbor_veto =', \
multiples_code.neighbor_veto
print 'multiples_code.final_scale_factor =', \
multiples_code.final_scale_factor
print 'multiples_code.initial_scatter_factor =', \
multiples_code.initial_scatter_factor
print 'multiples_code.final_scatter_factor =', \
multiples_code.final_scatter_factor
print 'multiples_code.retain_binary_apocenter =', \
multiples_code.retain_binary_apocenter
print 'multiples_code.wide_perturbation_limit =', \
multiples_code.wide_perturbation_limit
pre = "%%% "
E0,cpu0 = print_log(pre, time, multiples_code)
while time < end_time:
time += delta_t
multiples_code.evolve_model(time)
# Copy values from the module to the set in memory.
channel.copy()
# Copy the index (ID) as used in the module to the id field in
# memory. The index is not copied by default, as different
# codes may have different indices for the same particle and
# we don't want to overwrite silently.
channel.copy_attribute("index_in_code", "id")
print_log(pre, time, multiples_code, E0, cpu0)
sys.stdout.flush()
#-----------------------------------------------------------------
if not outfile == None:
# Write data to a file.
f = open(outfile, 'w')
#--------------------------------------------------
# Need to save top-level stellar data and parameters.
# Need to save multiple data and parameters.
f.write('%.15g\n'%(time.number))
for s in multiples_code.stars: write_star(s, f)
#--------------------------------------------------
f.close()
print 'wrote file', outfile
print ''
gravity.stop()
def compress_binary_components(comp1, comp2, scale):
# Compress the two-body system consisting of comp1 and comp2 to
# lie within distance scale of one another.
pos1 = comp1.position
pos2 = comp2.position
sep12 = ((pos2-pos1)**2).sum()
if sep12 > scale*scale:
print '\ncompressing components', int(comp1.id.number), \
'and', int(comp2.id.number), 'to separation', scale.number
sys.stdout.flush()
mass1 = comp1.mass
mass2 = comp2.mass
total_mass = mass1 + mass2
vel1 = comp1.velocity
vel2 = comp2.velocity
cmpos = (mass1*pos1+mass2*pos2)/total_mass
cmvel = (mass1*vel1+mass2*vel2)/total_mass
# For now, create and delete a temporary kepler
# process to handle the transformation. Obviously
# more efficient to define a single kepler at the
# start of the calculation and reuse it.
kep = Kepler(redirection = "none")
kep.initialize_code()
mass = comp1.mass + comp2.mass
rel_pos = pos2 - pos1
rel_vel = vel2 - vel1
kep.initialize_from_dyn(mass,
rel_pos[0], rel_pos[1], rel_pos[2],
rel_vel[0], rel_vel[1], rel_vel[2])
M,th = kep.get_angles()
a,e = kep.get_elements()
if e < 1:
peri = a*(1-e)
apo = a*(1+e)
else:
peri = a*(e-1)
apo = 2*a # OK - used ony to reset scale
limit = peri + 0.01*(apo-peri)
if scale < limit: scale = limit
if M < 0:
# print 'approaching'
kep.advance_to_periastron()
kep.advance_to_radius(limit)
else:
# print 'receding'
if kep.get_separation() < scale:
kep.advance_to_radius(limit)
else:
kep.return_to_radius(scale)
# a,e = kep.get_elements()
# r = kep.get_separation()
# E,J = kep.get_integrals()
# print 'kepler: a,e,r =', a.number, e.number, r.number
# print 'E, J =', E, J
# Note: if periastron > scale, we are now just past periastron.
new_rel_pos = kep.get_separation_vector()
new_rel_vel = kep.get_velocity_vector()
kep.stop()
# Enew = 0
# r2 = 0
# for k in range(3):
# Enew += 0.5*(new_rel_vel[k].number)**2
# r2 += (new_rel_pos[k].number)**2
# rnew = math.sqrt(r2)
# Enew -= mass.number/r1
# print 'E, Enew, rnew =', E.number, E1, r1
# Problem: the vectors returned by kepler are lists,
# not numpy arrays, and it looks as though we can say
# comp1.position = pos, but not comp1.position[k] =
# xxx, as we'd like... Also, we don't know how to
# copy a numpy array with units... TODO
newpos1 = pos1 - pos1 # stupid trick to create zero vectors
newpos2 = pos2 - pos2 # with the proper form and units...
newvel1 = vel1 - vel1
newvel2 = vel2 - vel2
frac2 = mass2/total_mass
for k in range(3):
dxk = new_rel_pos[k]
dvk = new_rel_vel[k]
newpos1[k] = cmpos[k] - frac2*dxk
newpos2[k] = cmpos[k] + (1-frac2)*dxk
newvel1[k] = cmvel[k] - frac2*dvk
newvel2[k] = cmvel[k] + (1-frac2)*dvk
# Perform the changes to comp1 and comp2, and recursively
# transmit them to the (currently absolute) coordinates of
# all lower components.
offset_particle_tree(comp1, newpos1-pos1, newvel1-vel1)
offset_particle_tree(comp2, newpos2-pos2, newvel2-vel2)
def CutOrAdvance(enc_bodies, primary_sysID, converter=None):
bodies = enc_bodies.copy()
if converter==None:
converter = nbody_system.nbody_to_si(bodies.mass.sum(), 2 * np.max(bodies.radius.number) | bodies.radius.unit)
systems = stellar_systems.get_heirarchical_systems_from_set(bodies, converter=converter, RelativePosition=False)
# Deal with Possible Key Issues with Encounters with 3+ Star Particles Being Run More than Other Systems ...
if int(primary_sysID) not in systems.keys():
print "...: Error: Previously run binary system has been found! Not running this system ..."
print primary_sysID
print systems.keys()
print "---------------------------------"
return None
# As this function is pulling from Multiples, there should never be more or less than 2 "Root" Particles ...
if len(systems) != 2:
print "...: Error: Encounter has more roots than expected! Total Root Particles:", len(systems)
print bodies
print "---------------------------------"
return None
# Assign the Primary System to #1 and Perturbing System to #2
sys_1 = systems[int(primary_sysID)]
secondary_sysID = [key for key in systems.keys() if key!=int(primary_sysID)][0]
sys_2 = systems[secondary_sysID]
print 'All System Keys:', systems.keys()
print 'Primary System Key:', primary_sysID
print 'System 1 IDs:', sys_1.id
print 'System 2 IDs:', sys_2.id
# Calculate Useful Quantities
mass_ratio = sys_2.mass.sum()/sys_1.mass.sum()
total_mass = sys_1.mass.sum() + sys_2.mass.sum()
rel_pos = sys_1.center_of_mass() - sys_2.center_of_mass()
rel_vel = sys_1.center_of_mass_velocity() - sys_2.center_of_mass_velocity()
# Initialize Kepler Worker
kep = Kepler(unit_converter = converter, redirection = 'none')
kep.initialize_code()
kep.initialize_from_dyn(total_mass, rel_pos[0], rel_pos[1], rel_pos[2], rel_vel[0], rel_vel[1], rel_vel[2])
# Check to See if the Periastron is within the Ignore Distance for 10^3 Perturbation
p = kep.get_periastron()
ignore_distance = mass_ratio**(1./3.) * 600 | units.AU
if p > ignore_distance:
print "Encounter Ignored due to Periastron of", p.in_(units.AU), "and an IgnoreDistance of",ignore_distance
kep.stop()
print "---------------------------------"
return None
# Move the Particles to be Relative to their Respective Center of Mass
cm_sys_1, cm_sys_2 = sys_1.center_of_mass(), sys_2.center_of_mass()
cmv_sys_1, cmv_sys_2 = sys_1.center_of_mass_velocity(), sys_2.center_of_mass_velocity()
for particle in sys_1:
particle.position -= cm_sys_1
particle.velocity -= cmv_sys_1
for particle in sys_2:
particle.position -= cm_sys_2
particle.velocity -= cmv_sys_2
# Check to See if the Planets are Closer than the Ignore Distance
# Note: This shouldn't happen in the main code, but this prevents overshooting the periastron in debug mode.
if kep.get_separation() > ignore_distance:
kep.advance_to_radius(ignore_distance)
# Advance the Center of Masses to the Desired Distance in Reduced Mass Coordinates
x, y, z = kep.get_separation_vector()
rel_pos_f = rel_pos.copy()
rel_pos_f[0], rel_pos_f[1], rel_pos_f[2] = x, y, z
vx, vy, vz = kep.get_velocity_vector()
rel_vel_f = rel_vel.copy()
rel_vel_f[0], rel_vel_f[1], rel_vel_f[2] = vx, vy, vz
# Transform to Absolute Coordinates from Kepler Reduced Mass Coordinates
cm_pos_1, cm_pos_2 = sys_2.mass.sum() * rel_pos_f / total_mass, -sys_1.mass.sum() * rel_pos_f / total_mass
cm_vel_1, cm_vel_2 = sys_2.mass.sum() * rel_vel_f / total_mass, -sys_1.mass.sum() * rel_vel_f / total_mass
# Move the Particles to the New Postions of their Respective Center of Mass
for particle in sys_1:
particle.position += cm_pos_1
particle.velocity += cm_vel_1
for particle in sys_2:
particle.position += cm_pos_2
particle.velocity += cm_vel_2
# Stop Kepler and Return the Systems as a Particle Set
kep.stop()
# Collect the Collective Particle Set to be Returned Back
final_set = Particles()
final_set.add_particles(sys_1)
final_set.add_particles(sys_2)
print "---------------------------------"
return final_set
def run_ph4(options,
time=None,
stars=None,
mc_root_to_tree=None,
randomize=True):
infile = options.infile
outfile = options.outfile
restart_file = options.restart_file
number_of_stars = options.N
number_of_binaries = options.Nbin
end_time = options.t_end | nbody_system.time
delta_t = options.delta_t | nbody_system.time
n_workers = options.n_workers
use_gpu = options.use_gpu
gpu_worker = options.gpu_worker
salpeter = options.salpeter
accuracy_parameter = options.accuracy_parameter
softening_length = options.softening_length | nbody_system.length
manage_encounters = options.manage_encounters
random_seed = options.random_seed
if randomize:
if random_seed <= 0:
numpy.random.seed()
random_seed = numpy.random.randint(1, pow(2, 31) - 1)
numpy.random.seed(random_seed)
print "random seed =", random_seed
if infile is not None: print "input file =", infile
if restart_file is not None: print "restart file =", restart_file
if restart_file is not None and infile is not None:
print "restart file overrides input file"
print "end_time =", end_time.number
print "delta_t =", delta_t.number
print "n_workers =", n_workers
print "use_gpu =", use_gpu
print "manage_encounters =", manage_encounters
print "n =", number_of_stars
print "nbin=", number_of_binaries
print "\ninitializing the gravity module"
sys.stdout.flush()
init_smalln()
# Note that there are actually three GPU options:
#
# 1. use the GPU code and allow GPU use (default)
# 2. use the GPU code but disable GPU use (-g)
# 3. use the non-GPU code (-G)
if gpu_worker == 1:
try:
#gravity = GravityModule(number_of_workers = n_workers,
# redirection = "xterm")
gravity = GravityModule(number_of_workers=n_workers,
redirection="none",
mode="gpu")
except Exception as ex:
gravity = GravityModule(number_of_workers=n_workers,
redirection="none")
else:
gravity = GravityModule(number_of_workers=n_workers,
redirection="none")
gravity.initialize_code()
gravity.parameters.set_defaults()
if softening_length < 0.0 | nbody_system.length:
# Use ~interparticle spacing. Assuming standard units here. TODO
eps2 = 0.25*(float(number_of_stars))**(-0.666667) \
| nbody_system.length**2
else:
eps2 = softening_length * softening_length
print 'softening length =', eps2.sqrt()
gravity.parameters.timestep_parameter = accuracy_parameter
gravity.parameters.epsilon_squared = eps2
gravity.parameters.use_gpu = use_gpu
kep = Kepler(redirection="none")
kep.initialize_code()
multiples_code = None
Xtra = numpy.zeros(2)
#-----------------------------------------------------------------
if (restart_file is None
or not os.path.exists(restart_file + ".stars.hdf5")
) and infile is None and stars is None:
print "making a Plummer model"
stars = new_plummer_model(number_of_stars)
id = numpy.arange(number_of_stars)
stars.id = id + 1
print "setting particle masses and radii"
if salpeter == 0:
print 'equal masses'
total_mass = 1.0 | nbody_system.mass
scaled_mass = total_mass / number_of_stars
else:
print 'salpeter mass function'
scaled_mass = new_salpeter_mass_distribution_nbody(number_of_stars)
stars.mass = scaled_mass
print "centering stars"
stars.move_to_center()
print "scaling stars to virial equilibrium"
stars.scale_to_standard(
smoothing_length_squared=gravity.parameters.epsilon_squared)
time = 0.0 | nbody_system.time
total_mass = stars.mass.sum()
ke = pa.kinetic_energy(stars)
kT = ke / (1.5 * number_of_stars)
# Set dynamical radii (assuming virial equilibrium and standard
# units). Note that this choice should be refined, and updated
# as the system evolves. Probably the choice of radius should be
# made entirely in the multiples module. TODO. In these units,
# M = 1 and <v^2> = 0.5, so the mean 90-degree turnaround impact
# parameter is
#
# b_90 = G (m_1+m_2) / vrel^2
# = 2 <m> / 2<v^2>
# = 2 / N for equal masses
#
# Taking r_i = m_i / 2<v^2> = m_i in virial equilibrium means
# that, approximately, "contact" means a 90-degree deflection (r_1
# + r_2 = b_90). A more conservative choice with r_i less than
# this value will isolates encounters better, but also place more
# load on the large-N dynamical module.
stars.radius = stars.mass.number | nbody_system.length
if number_of_binaries > 0:
# Turn selected stars into binary components.
# Only tested for equal-mass case.
added_mass = 0.0 | nbody_system.mass
# Work with energies rather than semimajor axes.
Emin = 10 * kT
Emax = 20 * kT
ecc = 0.1
id_count = number_of_stars
nbin = 0
for i in range(0, number_of_stars,
number_of_stars / number_of_binaries):
# Star i is CM, becomes component, add other star at end.
nbin += 1
mass = stars[i].mass
#new_mass = numpy.random.uniform()*mass # uniform q?
new_mass = mass # uniform q?
mbin = mass + new_mass
fac = new_mass / mbin
E = Emin + numpy.random.uniform() * (Emax - Emin)
a = 0.5 * nbody_system.G * mass * new_mass / E
kep.initialize_from_elements(mbin, a, ecc)
dr = quantities.AdaptingVectorQuantity()
dr.extend(kep.get_separation_vector())
dv = quantities.AdaptingVectorQuantity()
dv.extend(kep.get_velocity_vector())
newstar = datamodel.Particles(1)
newstar.mass = new_mass
newstar.position = stars[i].position + (1 - fac) * dr
newstar.velocity = stars[i].velocity + (1 - fac) * dv
newstar.radius = newstar.mass.number | nbody_system.length
#newstar.radius = 3.0*stars[i].radius # HACK: try to force collision
# stars[i].mass = mass
stars[i].position = stars[i].position - fac * dr
stars[i].velocity = stars[i].velocity - fac * dv
id_count += 1
newstar.id = id_count
stars.add_particles(newstar)
added_mass += new_mass
if nbin >= number_of_binaries: break
kep.stop()
print 'created', nbin, 'binaries'
sys.stdout.flush()
stars.mass = stars.mass * total_mass / (total_mass + added_mass)
number_of_stars += nbin
Xtra = numpy.zeros(2)
print "recentering stars"
stars.move_to_center()
sys.stdout.flush()
stars.savepoint(time)
print ''
print "adding particles"
# print stars
sys.stdout.flush()
gravity.particles.add_particles(stars)
gravity.commit_particles()
else:
print "Restart detected. Loading parameters from restart."
new_end = options.t_end
stars, time, multiples_code, Xtra = MRest.read_state_from_file(
restart_file, gravity, new_smalln, kep)
options.t_end = new_end
total_mass = stars.mass.sum()
ke = pa.kinetic_energy(stars)
kT = ke / (1.5 * number_of_stars)
# print "IDs:", stars.id.number
print ''
print "number_of_stars =", number_of_stars
print "evolving to time =", end_time.number, \
"in steps of", delta_t.number
sys.stdout.flush()
# Channel to copy values from the code to the set in memory.
channel = gravity.particles.new_channel_to(stars)
stopping_condition = gravity.stopping_conditions.collision_detection
stopping_condition.enable()
# -----------------------------------------------------------------
# Create the coupled code and integrate the system to the desired
# time, managing interactions internally.
kep = init_kepler(stars[0], stars[1])
if not multiples_code:
multiples_code = multiples.Multiples(gravity, new_smalln, kep)
multiples_code.neighbor_distance_factor = 1.0
multiples_code.neighbor_veto = True
#multiples_code.neighbor_distance_factor = 2.0
#multiples_code.neighbor_veto = True
multiples_code.retain_binary_apocenter = False
print ''
print 'multiples_code.initial_scale_factor =', \
multiples_code.initial_scale_factor
print 'multiples_code.neighbor_distance_factor =', \
multiples_code.neighbor_distance_factor
print 'multiples_code.neighbor_veto =', \
multiples_code.neighbor_veto
print 'multiples_code.final_scale_factor =', \
multiples_code.final_scale_factor
print 'multiples_code.initial_scatter_factor =', \
multiples_code.initial_scatter_factor
print 'multiples_code.final_scatter_factor =', \
multiples_code.final_scatter_factor
print 'multiples_code.retain_binary_apocenter =', \
multiples_code.retain_binary_apocenter
# if mc_root_to_tree is not None:
# multiples_code.root_to_tree = mc_root_to_tree
# print 'multiples code re-loaded with binary trees snapshot'
pre = "%%% "
E0, cpu0 = print_log(pre, time, multiples_code)
while time < end_time:
time += delta_t
multiples_code.evolve_model(time)
# Copy values from the module to the set in memory.
channel.copy()
# Copy the index (ID) as used in the module to the id field in
# memory. The index is not copied by default, as different
# codes may have different indices for the same particle and
# we don't want to overwrite silently.
channel.copy_attribute("index_in_code", "id")
print_log(pre, time, multiples_code, E0, cpu0)
stars.savepoint(time)
MRest.write_state_to_file(time,
stars,
gravity,
multiples_code,
options.restart_file,
Xtra,
backup=1)
sys.stdout.flush()
#-----------------------------------------------------------------
if not outfile is None:
# Write data to a file.
f = open(outfile, 'w')
#--------------------------------------------------
# Need to save top-level stellar data and parameters.
# Need to save multiple data and parameters.
f.write('%.15g\n' % time.number)
for s in multiples_code.stars:
write_star(s, f)
#--------------------------------------------------
f.close()
print 'wrote file', outfile
print ''
gravity.stop()
def compress_binary_components(comp1, comp2, scale):
# Compress the two-body system consisting of comp1 and comp2 to
# lie within distance scale of one another.
pos1 = comp1.position
pos2 = comp2.position
sep12 = ((pos2 - pos1)**2).sum()
if sep12 > scale * scale:
print('\ncompressing components', int(comp1.id.number), \
'and', int(comp2.id.number), 'to separation', scale.number)
sys.stdout.flush()
mass1 = comp1.mass
mass2 = comp2.mass
total_mass = mass1 + mass2
vel1 = comp1.velocity
vel2 = comp2.velocity
cmpos = (mass1 * pos1 + mass2 * pos2) / total_mass
cmvel = (mass1 * vel1 + mass2 * vel2) / total_mass
# For now, create and delete a temporary kepler
# process to handle the transformation. Obviously
# more efficient to define a single kepler at the
# start of the calculation and reuse it.
kep = Kepler(redirection="none")
kep.initialize_code()
mass = comp1.mass + comp2.mass
rel_pos = pos2 - pos1
rel_vel = vel2 - vel1
kep.initialize_from_dyn(mass, rel_pos[0], rel_pos[1], rel_pos[2],
rel_vel[0], rel_vel[1], rel_vel[2])
M, th = kep.get_angles()
a, e = kep.get_elements()
if e < 1:
peri = a * (1 - e)
apo = a * (1 + e)
else:
peri = a * (e - 1)
apo = 2 * a # OK - used ony to reset scale
limit = peri + 0.01 * (apo - peri)
if scale < limit: scale = limit
if M < 0:
# print 'approaching'
kep.advance_to_periastron()
kep.advance_to_radius(limit)
else:
# print 'receding'
if kep.get_separation() < scale:
kep.advance_to_radius(limit)
else:
kep.return_to_radius(scale)
# a,e = kep.get_elements()
# r = kep.get_separation()
# E,J = kep.get_integrals()
# print 'kepler: a,e,r =', a.number, e.number, r.number
# print 'E, J =', E, J
# Note: if periastron > scale, we are now just past periastron.
new_rel_pos = kep.get_separation_vector()
new_rel_vel = kep.get_velocity_vector()
kep.stop()
# Enew = 0
# r2 = 0
# for k in range(3):
# Enew += 0.5*(new_rel_vel[k].number)**2
# r2 += (new_rel_pos[k].number)**2
# rnew = math.sqrt(r2)
# Enew -= mass.number/r1
# print 'E, Enew, rnew =', E.number, E1, r1
# Problem: the vectors returned by kepler are lists,
# not numpy arrays, and it looks as though we can say
# comp1.position = pos, but not comp1.position[k] =
# xxx, as we'd like... Also, we don't know how to
# copy a numpy array with units... TODO
newpos1 = pos1 - pos1 # stupid trick to create zero vectors
newpos2 = pos2 - pos2 # with the proper form and units...
newvel1 = vel1 - vel1
newvel2 = vel2 - vel2
frac2 = mass2 / total_mass
for k in range(3):
dxk = new_rel_pos[k]
dvk = new_rel_vel[k]
newpos1[k] = cmpos[k] - frac2 * dxk
newpos2[k] = cmpos[k] + (1 - frac2) * dxk
newvel1[k] = cmvel[k] - frac2 * dvk
newvel2[k] = cmvel[k] + (1 - frac2) * dvk
# Perform the changes to comp1 and comp2, and recursively
# transmit them to the (currently absolute) coordinates of
# all lower components.
offset_particle_tree(comp1, newpos1 - pos1, newvel1 - vel1)
offset_particle_tree(comp2, newpos2 - pos2, newvel2 - vel2)
def get_orbit_ini(m0, m1, peri, ecc, incl, omega,
rel_force=0.01, r_disk=50|units.AU):
converter=nbody_system.nbody_to_si(1|units.MSun,1|units.AU)
# semi-major axis
if ecc!=1.0:
semi = peri/(1.0-ecc)
else:
semi = 1.0e10 | units.AU
# relative position and velocity vectors at the pericenter using kepler
kepler = Kepler_twobody(converter)
kepler.initialize_code()
kepler.initialize_from_elements(mass=(m0+m1), semi=semi, ecc=ecc, periastron=peri) # at pericenter
# moving particle backwards to radius r where: F_m1(r) = rel_force*F_m0(r_disk)
#r_disk = peri
r_ini = r_disk*(1.0 + numpy.sqrt(m1/m0)/rel_force)
kepler.return_to_radius(radius=r_ini)
rl = kepler.get_separation_vector()
r = [rl[0].value_in(units.AU), rl[1].value_in(units.AU), rl[2].value_in(units.AU)] | units.AU
vl = kepler.get_velocity_vector()
v = [vl[0].value_in(units.kms), vl[1].value_in(units.kms), vl[2].value_in(units.kms)] | units.kms
period_kepler = kepler.get_period()
time_peri = kepler.get_time()
kepler.stop()
# rotation of the orbital plane by inclination and argument of periapsis
a1 = ([1.0, 0.0, 0.0], [0.0, numpy.cos(incl), -numpy.sin(incl)], [0.0, numpy.sin(incl), numpy.cos(incl)])
a2 = ([numpy.cos(omega), -numpy.sin(omega), 0.0], [numpy.sin(omega), numpy.cos(omega), 0.0], [0.0, 0.0, 1.0])
rot = numpy.dot(a1,a2)
r_au = numpy.reshape(r.value_in(units.AU), 3, 1)
v_kms = numpy.reshape(v.value_in(units.kms), 3, 1)
r_rot = numpy.dot(rot, r_au) | units.AU
v_rot = numpy.dot(rot, v_kms) | units.kms
bodies = Particles(2)
bodies[0].mass = m0
bodies[0].radius = 1.0|units.RSun
bodies[0].position = (0,0,0) | units.AU
bodies[0].velocity = (0,0,0) | units.kms
bodies[1].mass = m1
bodies[1].radius = 1.0|units.RSun
bodies[1].x = r_rot[0]
bodies[1].y = r_rot[1]
bodies[1].z = r_rot[2]
bodies[1].vx = v_rot[0]
bodies[1].vy = v_rot[1]
bodies[1].vz = v_rot[2]
bodies.age = 0.0 | units.yr
bodies.move_to_center()
print "\t r_rel_ini = ", r_rot.in_(units.AU)
print "\t v_rel_ini = ", v_rot.in_(units.kms)
print "\t time since peri = ", time_peri.in_(units.yr)
a_orbit, e_orbit, p_orbit = orbital_parameters(r_rot, v_rot, (m0+m1))
print "\t a = ", a_orbit.in_(units.AU), "\t e = ", e_orbit, "\t period = ", p_orbit.in_(units.yr)
return bodies, time_peri
def get_orbit_ini(m0,
m1,
peri,
ecc,
incl,
omega,
rel_force=0.01,
r_disk=50 | units.AU):
converter = nbody_system.nbody_to_si(1 | units.MSun, 1 | units.AU)
# semi-major axis
if ecc != 1.0:
semi = peri / (1.0 - ecc)
else:
semi = 1.0e10 | units.AU
# relative position and velocity vectors at the pericenter using kepler
kepler = Kepler_twobody(converter)
kepler.initialize_code()
kepler.initialize_from_elements(mass=(m0 + m1),
semi=semi,
ecc=ecc,
periastron=peri) # at pericenter
# moving particle backwards to radius r where: F_m1(r) = rel_force*F_m0(r_disk)
#r_disk = peri
r_ini = r_disk * (1.0 + numpy.sqrt(m1 / m0) / rel_force)
kepler.return_to_radius(radius=r_ini)
rl = kepler.get_separation_vector()
r = [
rl[0].value_in(units.AU), rl[1].value_in(units.AU), rl[2].value_in(
units.AU)
] | units.AU
vl = kepler.get_velocity_vector()
v = [
vl[0].value_in(units.kms), vl[1].value_in(units.kms), vl[2].value_in(
units.kms)
] | units.kms
period_kepler = kepler.get_period()
time_peri = kepler.get_time()
kepler.stop()
# rotation of the orbital plane by inclination and argument of periapsis
a1 = ([1.0, 0.0,
0.0], [0.0, numpy.cos(incl),
-numpy.sin(incl)], [0.0,
numpy.sin(incl),
numpy.cos(incl)])
a2 = ([numpy.cos(omega), -numpy.sin(omega),
0.0], [numpy.sin(omega), numpy.cos(omega), 0.0], [0.0, 0.0, 1.0])
rot = numpy.dot(a1, a2)
r_au = numpy.reshape(r.value_in(units.AU), 3, 1)
v_kms = numpy.reshape(v.value_in(units.kms), 3, 1)
r_rot = numpy.dot(rot, r_au) | units.AU
v_rot = numpy.dot(rot, v_kms) | units.kms
bodies = Particles(2)
bodies[0].mass = m0
bodies[0].radius = 1.0 | units.RSun
bodies[0].position = (0, 0, 0) | units.AU
bodies[0].velocity = (0, 0, 0) | units.kms
bodies[1].mass = m1
bodies[1].radius = 1.0 | units.RSun
bodies[1].x = r_rot[0]
bodies[1].y = r_rot[1]
bodies[1].z = r_rot[2]
bodies[1].vx = v_rot[0]
bodies[1].vy = v_rot[1]
bodies[1].vz = v_rot[2]
bodies.age = 0.0 | units.yr
bodies.move_to_center()
print "\t r_rel_ini = ", r_rot.in_(units.AU)
print "\t v_rel_ini = ", v_rot.in_(units.kms)
print "\t time since peri = ", time_peri.in_(units.yr)
a_orbit, e_orbit, p_orbit = orbital_parameters(r_rot, v_rot, (m0 + m1))
print "\t a = ", a_orbit.in_(
units.AU), "\t e = ", e_orbit, "\t period = ", p_orbit.in_(units.yr)
return bodies, time_peri
