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mcluster.ini
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mcluster.ini
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#_____________________________________________________________________________________
[Mcluster]
# initial number of objects for each sub-population:
# - defined as n = ns + nb, where ns - number of single stars, nb - number
# of binaries. Thus total number of stars is equal to ns + 2 * nb
# - if only one values is defined here, only one populations is read
# - default value: 100000
n = 100000
# reference binary fraction
# - binary fraction for the reference population to compute the number of
# objects in the simulated population with different binary fractions. The
# simulated population will have the same mass as the reference population
# The reference population has IMFs and a number of objects as defined
# below in the mocca.ini file, except the binary fraction defined as the
# primordial binary fraction. The new numbers of objects for the simulated
# population are listed in the model-scale.dat file.
# !! CAUTION - if the binary fractions for the reference and primordial binary
# fractions are the same all parameters listed below are not changed and the
# simulated model has binary fraction as given in the reference binary fraction
# - default value: 0.95, 0.95
fracb_reference = 0.95
# primordial binary fraction:
# - number of binaries (nb) is calculated as nb = fracb * n
# - if fracb > 0 - there are primordial binaries
# - if fracb = 0 - there are only binaries created dynamically
# - default value: 0.2
fracb = 0.95
# initial model:
# 0 - homogeneous sphere
# 1 - Plummer
# 2 - King
# 3 - Subr
# - default value: 1
initialModel = 2
# Kind model parameter:
# - minimum = 1.0, maximum = 12.0
# - default value: 5.0
w0 = 6.0
# mass segregation:
# 0.0 - unsegregated
# 1.0 - completely segregated
# - take maximally S=0.99 for profile=2
# - default value: 0.0
S = 0.0, 0.0
# fractal dimension (2^D children per parent):
# if fractal > 0: boxy distribution (Goodwin & Whitworth 2004)
# if fractal < 0: spherical distribution (Alex Livernois 2021)
# abs(fractal) values allowed:
# 3.0 - unfractal
# 2.6 - 2/8 fractal
# 2.0 - 4/8 fractal
# 1.6 - 6/8 fractal
# - default value: 3.0
fractal = 3.0, 3.0
# virial ratio:
# - qvir = 0.5 for equilibrium, <0.5 collapsing, >0.5 expanding
# - default value: 0.5
qvir_pop = 0.5
# virial ratio of the whole population:
# - qvir = 0.5 for equilibrium, <0.5 collapsing, >0.5 expanding
# - default value: 0.5
qvir = 0.5
# stellar mass function:
# 0 - equal masses equivalent to single_mass
# 1 - Kroupa (2001) mass function
# 2 - use multi power law (based on mufu.c by L.Subr)
# 3 - L3 IMF Maschberger (2012)
# - default value: 1
mfunc = 1, 1
# stellar mass in case of single-mass cluster:
# - default value: 1.0
single_mass = 1.0, 1.0
# lower mass limit for mfunc = 1 & mfunc = 3:
# - default value: 0.08
mlow = 0.08, 0.08
# upper mass limit for mfunc = 1 & mfunc = 3:
# - default value: 100.0
mup = 100.0, 100.0
# alpha slopes for mfunc = 2:
# - default value: -1.35, -2.35, -2.7, 0.0, 0.0
alpha_imf = [-1.50, -2.90, -2.7, 0.0, 0.0]
# mass limits for mfunc = 2:
# - default value: 0.08, 0.5, 4.0, 100, 0.0, 0.0
mlim_imf = [0.08, 0.5, 4.0, 100.0, 0.0, 0.0]
# alpha slope for mfunc = 3 (L3 mass function, Maschberger 2012):
# - default value: 2.3
alpha_L3 = 2.3, 2.3
# beta slope for mfunc = 3:
# - default value: 1.4
beta_L3 = 1.4, 1.4
# mu parameter for mfunc = 3:
# - default value: 0.2
mu_L3 = 0.2, 0.2
# pairing of binary components:
# 0 - random pairing
# 1 - ordered pairing for components with masses M>5Mo
# 2 - random but separate pairing for components with masses m>5Mo
# 3 - uniform distribution of mass ratio (0.1<q<1.0) for m>5Mo and random pairing
# for remaining (Kiminki & Kobulnicky 2012; Sana et al., 2012; Kobulnicky et al. 2014)
# - default value: 3
pairing = 3, 3
# semi-major axis distribution:
# 0 - uniform distribution in log(a), between amin and amax
# 1 - lognormal distribution distribution for a
# 2 - based on Kroupa (1995) period distribution
# 3 - based on Kroupa (1995) period distribution for M<5Mo;
# based on Sana et al. (2012); Oh, S., Kroupa, P., & Pflamm-Altenburg, J. (2015) period distribution for M>5Mo
# 4 - flat uniform distribution in a ranging from amin to amax
# 5 - based on Duquennoy & Mayor (1991) period distribution
# 6 - uniform distribution in log(a), between amin and amax for M<5Mo; Sana et al. (2012) period distribution for M>5Mo
# !! ALERT this will generate uniform distribution of mass ratio (0.1<q<1.0) for m>5Mo and also for m<5Mo indipendently from pairing !!
# - default value: 3
adis = 0, 6
# eigenevolution:
# 0 - off
# 1 - Kroupa (1995) eigenevolution for pre-main sequence short-period binaries and feeding algorithm !! ALERT this will set adis = 2 and pairing = 1 !!
# 2 - new eigenevolution and feeding algorithm - Kroupa 2013, rewieved in Belloni et al. (2017) !! ALERT this will set adis = 3 and pairing = 3 !!
# - default value: 0
eigen = 0, 0
# minimum binary semi-major axis:
# - defined in solar radii
# - if amin > 0 then amin = amin
# semimajor axis is considered if rperi >= 2.0 * (R1 + R2)
# go to line 4402 in McLuster to change it
# - if amin < 0: amin = -amin * (R1 + R2)/(1-e)
# amin * (R1 + R2) is the minimum allowed pericenter distance for each binary
# semimajor axis is considered if rperi >= abs(amin) * (R1 + R2)
# with R1 and R2 radii of the two binary stars and e the eccentricity
# - default value: -2.0
amin = -2.0
# maximum binary semi-major axis:
# - defined in solar radii
# - if amax >= 0 then amax = amax
# - if amax < 0: amax = -amax*(2.5*Rh/N) (soft, hard boundary for binaries; it consider only the total Rh and N)
# - default value: 10747.0 (= 50 AU) input in Rsun
amax = 10747.0, 10747.0
# tidal field:
# 0 - no tidal field
# 1 - point-mass galaxy
# 2 - Allen & Santillan
# 3 - Sverre's Nbody6 standard tidal field
# - default value: 0
tf = 1
# tidal radius [pc] (for the whole system):
# - for tf = 0, it is defined as the limiting radius for the initial model
# - for tf = 1, it is defined as the tidal radius for the whole system
# - if rbar < 0.0, abs(rbar) is the galactocentric distance RG in kpc and the tidal radius is determined
# according to the equation: (rbar/pc) = 0.31 (RG/kpc)^(2/3) (M/Mo)^(1/3)
# - default value: 35.8
rbar = 100.0
# galactocentric radius in pc:
# - used only if tf == 2
# - default value: 1000
galactocentric_radius = 1000
# cluster velocity in km/2:
# - used only if tf == 2
# - default value: 220
cluster_velocity = 220
# half mass radius [pc]:
# - if rh_mcl > 0.0 it is considered for the whole cluster
# - if rh_mcl < 0.0 it is considered for the first population
#
# - if abs(rh_mcl) > 1.d9 the model is not underfilled (standard King model, for Plummer model it will set Rh=0.1*Rt)
# - if abs(rh_mcl) < 1.d9 the model is underfilled by a rplum factor, defined as rplum = rbar/rh_mcl
#
# - the scaling parameter to physical units is determined from rh_mcl
# - !! ALERT rh_mcl cannot be smaller than 0 for single population
# - default value: 1.0
rh_mcl = 1.0
# Concentration radius parameter:
# - defined as Rh_i/Rh1, the ratio between the half-mass radii of the i-th and the first generation),
# - the first value is Rh2/Rh1 (the ratio between the half-mass radii of the second and the first generation)
# - the second value would be Rh3/Rh1 (the ratio between the half-mass radii of the third and the first generation)
# - it will be skipped for single stellar population
# - default value: 0.5
conc_pop = 0.5
# Scaling first population only:
# - if set to 1, the Jeans equation for multiple stellar populations are not solved
# - the velocities of the second population are normalized by a factor vscale2/vscale1
# - the scaling parameter are defined for the first population only (mscale, rscale, vscale)
# - CAUTION if set to 1, rh_mcl has to be < 0
# - default value: 0
scaling_1pop_only = 0
# Different epoch for pop2
# - the epoch time for pop2 is different for different mass range
# - the time step for each mass range is increased of
# - time_step = delta_formation_pop2/(number_of_mass_range - 1)
# - applied only if delta_formation_pop2 > 0.0
# - default value: 0.0
delta_formation_pop2 = 0.0
# Mass range for different epoch for pop2
# - the epoch time for pop2 is different for different mass range
# - the time step for each mass range is increased of
# - time_step = delta_formation_pop2/(number_of_mass_range - 1)
# - default value: 0.08, 0.5, 4.0, 100.0, 0.0, 0.0
mass_range_delta_formation_pop2 = 0.08, 0.5, 4.0, 100.0, 0.0, 0.0
# potential energy valuation:
# - 0 - potential energy valuated as sum of gravitational potential for every object (~ N^2)
# - 1 - potential energy valuated in spherical symmetry (~ N)
# - default value: 1
potential_energy = 1
# age of population (in Myr):
# - default value: 0
epoch = 100.0, 0.0
# initial metallicity:
# - solar metallicity is z = 0.02
# - e.g. for M4 z = 0.002 (1/10 of the solar metallicity), and for
# NGC6397 z = 0.0002 (1/100 of the solar metallicity)
# - default value: 0.001
zini = 0.001, 0.001
# initial integer number to start random number generator for Mcluster initial conditions:
# - if it is set to 0, the seedmc is started with the current time
# - default value: 10
seedmc = 10
# output format:
# - 0 - single nbody.dat and binary nbody.dat for MOCCA simulations. The structure of those files are:
# - single - mass [M ], x, y, z, Vx, Vy, Vz [N-body units], age, metallicty, index of the population
# - binary - e, a [log10(Ro)], m1 [M ], m2 [M ], x, y, z, Vx, Vy, Vz [binary centerof mass, N-body units], age, metallicity, index of the population
# - 1 - standard dat.10 file for NBODY simulations. The structure of the file is:
# - binaries in the beginning of the file, i.e. 2 x NBIN lines with the binary individual masses + positions + velocities in the cluster frame
# - remaining single star lines, with mass + position + velocities in the cluster frame
# - All the data in N-body units
# - 2 - initial files for MOCCA & NBODY simulations will be generated at the same time
# - default value: 0
outputf = 2
# Make energy check at end of Mcluster:
# - 0 - off
# - 1 - on
# - default value: 1
check_en = 0
# Activate SSE/BSE for stellar/binary evolution:
# - 0 - off
# - 1 - on
# !! ALERT this will not be activated if outputf=0 or outputf=2 !!
# - default value: 0
BSE = 0