The full list of command line options is viewed with `--help` option. Default
values are given in brackets.

```sh
./freddi --help
```

expand

```
Freddi: numerical calculation of accretion disk evolution:

General options::
-h [ --help ] Produce help message

--config arg Set filepath for additional configuration
file. There is no need to declare a
configuration file with the default name
freddi.ini

--prefix arg (=freddi) Set prefix for output filenames. Output file
with distribution of parameters over time is
PREFIX.dat

--stdout Output temporal distribution to stdout
instead of PREFIX.dat file

-d [ --dir ] arg (=.) Choose the directory to write output files.
It should exist

--precision arg (=12) Number of digits to print into output files

--tempsparsity arg (=1) Output every k-th time moment

--fulldata Output files PREFIX_%d.dat with radial
structure for every time step. Default is to
output only PREFIX.dat with global disk
parameters for every time step

Basic binary and disk parameters
:
-a [ --alpha ] arg Alpha parameter of Shakura-Sunyaev model

--alphacold arg Alpha parameter of cold disk, currently it
is used only for the critical maximum value
of the surface density of the cold disk
Sigma_minus (Lasota et al., 2008, A&A 486,
523) and the cooling front velocity (Ludwig
et al., 1994, A&A 290, 473), see
--Qirr2Qvishot. Default value is --alpha
divided by ten

-M [ --Mx ] arg Mass of the central object, in the units of
solar masses

--kerr arg (=0) Dimensionless Kerr parameter of the black
hole

--Mopt arg Mass of the optical star, in units of solar
masses

--rochelobefill arg (=1) Dimensionless factor describing a size of
the optical star. Polar radius of the star
is rochelobefill * (polar radius of critical
Roche lobe)

--Topt arg (=0) Effective temperature of the optical star,
in units of Kelvins

-P [ --period ] arg Orbital period of the binary system, in
units of days

--rin arg Inner radius of the disk, in the units of
the gravitational radius of the central
object GM/c^2. There is no need to set it
for a neutron star. If it isn't set for a
black hole then the radius of ISCO orbit is
used, defined by --Mx and --kerr values

-R [ --rout ] arg Outer radius of the disk, in units of solar
radius. If it isn't set then the tidal
radius is used, defined by --Mx, --Mopt and
--period values as 90% of the Roche lobe
radius (Papaloizou & Pringle, 1977, MNRAS,
181, 441; see also Artymowicz & Lubow, 1994,
ApJ, 421, 651; http://xray.sai.msu.ru/~galja
/images/tidal_radius.pdf)

--risco arg Innermost stable circular orbit, in units of
gravitational radius of the central object
GM/c^2. If it isn't set then the radius of
ISCO orbit is used defined by --Mx and
--kerr values

Parameters of the disk model:
-O [ --opacity ] arg (=Kramers) Opacity law: Kramers (varkappa ~ rho /
T^7/2) or OPAL (varkappa ~ rho / T^5/2)

--Mdotout arg (=0) Accretion rate onto the disk through its
outer radius

--boundcond arg (=Teff) Outer-boundary movement condition

Values:
Teff: outer radius of the disk moves
inwards to keep photosphere temperature of
the disk larger than some value. This value
is specified by --Thot option
Tirr: outer radius of the disk moves
inwards to keep irradiation flux of the disk
larger than some value. The value of this
minimal irradiation flux is
[Stefan-Boltzmann constant] * Tirr^4, where
Tirr is specified by --Thot option

--Thot arg (=0) Minimum photosphere or irradiation
temperature at the outer edge of the hot
disk, Kelvin. For details see --boundcond
description

--Qirr2Qvishot arg (=0) Minimum Qirr / Qvis ratio at the outer edge
of the hot disk to switch the control over
the evolution of the hot disk radius: from
temperature-based regime to Sigma-based
cooling-front regime (see Lipunova et al.
(2021, Section 2.4) and Eq. A.1 in Lasota et
al. 2008; --alpha value is used for
Sigma_plus and --alphacold value is used for
Sigma_minus)

--initialcond arg (=powerF) Type of the initial condition for viscous
torque F or surface density Sigma

Values:
[NB! Here below dimensionless xi = (h -
h_in) / (h_out - h_in)]

powerF: F ~ xi^powerorder, powerorder is
specified by --powerorder option
linearF: F ~ xi, specific case of powerF
but can be normalised by --Mdot0, see its
description for details
powerSigma: Sigma ~ xi^powerorder,
powerorder is specified by --powerorder
option
sineF: F ~ sin( xi * pi/2 )
gaussF: F ~ exp(-(xi-mu)**2 / 2 sigma**2),
mu and sigma are specified by --gaussmu and
--gausssigma options
quasistat: F ~ f(h/h_out) * xi * h_out/h,
where f is quasi-stationary solution found
in Lipunova & Shakura 2000. f(xi=0) = 0,
df/dxi(xi=1) = 0

--F0 arg Initial maximum viscous torque in the disk,
dyn*cm. Can be overwritten via --Mdisk0 and
--Mdot0

--Mdisk0 arg Initial disk mass, g. If both --F0 and
--Mdisk0 are specified then --Mdisk0 is
used. If both --Mdot0 and --Mdisk0 are
specified then --Mdot0 is used

--Mdot0 arg Initial mass accretion rate through the
inner radius, g/s. If --F0, --Mdisk0 and
--Mdot0 are specified then --Mdot0 is used.
Works only when --initialcond is set to
linearF, sinusF or quasistat

--powerorder arg Parameter for the powerlaw initial condition
distribution. This option works only with
--initialcond=powerF or powerSigma

--gaussmu arg Position of the maximum for Gauss
distribution, positive number not greater
than unity. This option works only with
--initialcond=gaussF

--gausssigma arg Width of for Gauss distribution. This option
works only with --initialcond=gaussF

--windtype arg (=no) Type of the wind

no: no wind
SS73C: super-Eddington spherical wind from
Shakura-Sunyaev 1973
ShieldsOscil1986: toy wind model from
Shields et al. 1986 which was used to obtain
oscillations in the disk luminosity.
Requires --windC_w and --windR_w to be
specified
Janiuk2015: super-Eddington wind from
Janiuk et al 2015. Requires --windA_0 and
--windB_1 to be specified
Shields1986: thermal wind from Begelman et
al. 1983 and Shields et al. 1986. Requires
--windXi_max, --windT_ic and --windPow to be
specified
Woods1996AGN: thermal AGN wind from Woods
et al. 1996. Requires --windC_0 and
--windT_ic to be specified
Woods1996: thermal wind from Woods et al.
1996. Requires --windXi_max, --windT_ic and
--windPow to be specified
toy: a toy wind model used in
arXiv:2105.11974, the mass loss rate is
proportional to the central accretion rate.
Requires --windC_w to be specified

--windC_w arg The ratio of the mass loss rate due to wind
to the central accretion rate, |Mwind|/Macc

--windR_w arg The ratio of the wind launch radius to the
outer disk radius, Rwind/Rout

--windA_0 arg Dimensionless parameter characterizing the
strength of the super-Eddington wind in the
framework of the model Janiuk et al. 2015.
Effective value range from 10 to 25

--windB_1 arg The quantity is of the order of unity.
Characterizes the relationship between the
change in energy per particle and virial
energy.
E = B_1 * k * T

--windXi_max arg Ionization parameter, the ratio of the
radiation and gas pressures

--windT_ic arg Inverse Compton temperature, K.
Characterizes the hardness of the
irradiating spectrum

--windPow arg Multiplicative coefficient to control wind
power

--windC_0 arg Characteristic column density of the wind
mass loss rate from Woods et al. 1996 model,
g/(s*cm^2). For AGN approx value is 3e-13
g/(s*cm^2)

Parameters of self-irradiation:
Qirr = Cirr * (H/r / 0.05)^irrindex * L * psi / (4 pi R^2), where psi is the angular distribution of X-ray radiation
:
--Cirr arg (=0) Irradiation factor for the hot disk

--irrindex arg (=0) Irradiation index for the hot disk

--Cirrcold arg (=0) Irradiation factor for the cold disk

--irrindexcold arg (=0) Irradiation index for the cold disk

--h2rcold arg (=0) Semi-height to radius ratio for the cold
disk

--angulardistdisk arg (=plane) Angular distribution of the disk X-ray
radiation. Values: isotropic, plane

Parameters of flux calculation:
:
--colourfactor arg (=1.7) Colour factor to calculate X-ray flux

--emin arg (=1) Minimum energy of X-ray band, keV

--emax arg (=12) Maximum energy of X-ray band, keV

--staralbedo arg (=0) Part of X-ray radiation reflected by optical
star, (1 - albedo) heats star's photosphere.
Used only when --starflux is specified

-i [ --inclination ] arg (=0) Inclination of the system, degrees

--ephemerist0 arg (=0) Ephemeris for the time of the minimum of the
orbital light curve T0, phase zero
corresponds to inferior conjunction of the
optical star, days

--distance arg Distance to the system, kpc

--colddiskflux Add Fnu for cold disk into output file.
Default output is for hot disk only

--starflux Add Fnu for irradiated optical star into
output file. See --Topt, --starlod and
--h2rcold options. Default is output for the
hot disk only

--lambda arg Wavelength to calculate Fnu, Angstrom. You
can use this option multiple times. For each
lambda one additional column with values of
spectral flux density Fnu [erg/s/cm^2/Hz] is
produced

--passband arg Path of a file containing tabulated passband
for a photon counter detector, the first
column for wavelength in Angstrom, the
second column for transmission factor,
columns should be separated by spaces

Parameters of disk evolution calculation:
:
--inittime arg (=0) Initial time moment, days

-T [ --time ] arg Time interval to calculate evolution, days

--tau arg Time step, days

--Nx arg (=1000) Size of calculation grid

--gridscale arg (=log) Type of grid for angular momentum h: log or
linear

--starlod arg (=3) Level of detail of the optical star 3-D
model. The optical star is represented by a
triangular tile, the number of tiles is 20 *
4^starlod

```

```sh
./freddi-ns --help
```

expand

```
Freddi NS: numerical calculation of accretion disk evolution:

General options::
-h [ --help ] Produce help message

--config arg Set filepath for additional
configuration file. There is no need to
declare a configuration file with the
default name freddi.ini

--prefix arg (=freddi) Set prefix for output filenames. Output
file with distribution of parameters
over time is PREFIX.dat

--stdout Output temporal distribution to stdout
instead of PREFIX.dat file

-d [ --dir ] arg (=.) Choose the directory to write output
files. It should exist

--precision arg (=12) Number of digits to print into output
files

--tempsparsity arg (=1) Output every k-th time moment

--fulldata Output files PREFIX_%d.dat with radial
structure for every time step. Default
is to output only PREFIX.dat with
global disk parameters for every time
step

Basic binary and disk parameters
:
-a [ --alpha ] arg Alpha parameter of Shakura-Sunyaev
model

--alphacold arg Alpha parameter of cold disk, currently
it is used only for the critical
maximum value of the surface density of
the cold disk Sigma_minus (Lasota et
al., 2008, A&A 486, 523) and the
cooling front velocity (Ludwig et al.,
1994, A&A 290, 473), see
--Qirr2Qvishot. Default value is
--alpha divided by ten

-M [ --Mx ] arg Mass of the central object, in the
units of solar masses

--kerr arg (=0) Dimensionless Kerr parameter of the
black hole

--Mopt arg Mass of the optical star, in units of
solar masses

--rochelobefill arg (=1) Dimensionless factor describing a size
of the optical star. Polar radius of
the star is rochelobefill * (polar
radius of critical Roche lobe)

--Topt arg (=0) Effective temperature of the optical
star, in units of Kelvins

-P [ --period ] arg Orbital period of the binary system, in
units of days

--rin arg Inner radius of the disk, in the units
of the gravitational radius of the
central object GM/c^2. There is no need
to set it for a neutron star. If it
isn't set for a black hole then the
radius of ISCO orbit is used, defined
by --Mx and --kerr values

-R [ --rout ] arg Outer radius of the disk, in units of
solar radius. If it isn't set then the
tidal radius is used, defined by --Mx,
--Mopt and --period values as 90% of
the Roche lobe radius (Papaloizou &
Pringle, 1977, MNRAS, 181, 441; see
also Artymowicz & Lubow, 1994, ApJ,
421, 651; http://xray.sai.msu.ru/~galja
/images/tidal_radius.pdf)

--risco arg Innermost stable circular orbit, in
units of gravitational radius of the
central object GM/c^2. If it isn't set
then the radius of ISCO orbit is used
defined by --Mx and --kerr values

Parameters of the disk model:
-O [ --opacity ] arg (=Kramers) Opacity law: Kramers (varkappa ~ rho /
T^7/2) or OPAL (varkappa ~ rho / T^5/2)

--Mdotout arg (=0) Accretion rate onto the disk through
its outer radius

--boundcond arg (=Teff) Outer-boundary movement condition

Values:
Teff: outer radius of the disk moves
inwards to keep photosphere temperature
of the disk larger than some value.
This value is specified by --Thot
option
Tirr: outer radius of the disk moves
inwards to keep irradiation flux of the
disk larger than some value. The value
of this minimal irradiation flux is
[Stefan-Boltzmann constant] * Tirr^4,
where Tirr is specified by --Thot
option

--Thot arg (=0) Minimum photosphere or irradiation
temperature at the outer edge of the
hot disk, Kelvin. For details see
--boundcond description

--Qirr2Qvishot arg (=0) Minimum Qirr / Qvis ratio at the outer
edge of the hot disk to switch the
control over the evolution of the hot
disk radius: from temperature-based
regime to Sigma-based cooling-front
regime (see Lipunova et al. (2021,
Section 2.4) and Eq. A.1 in Lasota et
al. 2008; --alpha value is used for
Sigma_plus and --alphacold value is
used for Sigma_minus)

--initialcond arg (=powerF) Type of the initial condition for
viscous torque F or surface density
Sigma

Values:
[NB! Here below dimensionless xi = (h
- h_in) / (h_out - h_in)]

powerF: F ~ xi^powerorder, powerorder
is specified by --powerorder option
linearF: F ~ xi, specific case of
powerF but can be normalised by
--Mdot0, see its description for
details
powerSigma: Sigma ~ xi^powerorder,
powerorder is specified by --powerorder
option
sineF: F ~ sin( xi * pi/2 )
gaussF: F ~ exp(-(xi-mu)**2 / 2
sigma**2), mu and sigma are specified
by --gaussmu and --gausssigma options
quasistat: F ~ f(h/h_out) * xi *
h_out/h, where f is quasi-stationary
solution found in Lipunova & Shakura
2000. f(xi=0) = 0, df/dxi(xi=1) = 0
quasistat-ns: Distibution of the
initial viscous torque in the disc is
F = F0 * f_F(xi) * (1-h_in/h_out/xi) /
(1-h_in/h_out), where xi=h/h_out and
f_F(xi) is taken from Lipunova &
Shakura (2000)

--F0 arg Initial maximum viscous torque in the
disk, dyn*cm. Can be overwritten via
--Mdisk0 and --Mdot0

--Mdisk0 arg Initial disk mass, g. If both --F0 and
--Mdisk0 are specified then --Mdisk0 is
used. If both --Mdot0 and --Mdisk0 are
specified then --Mdot0 is used

--Mdot0 arg Initial mass accretion rate through the
inner radius, g/s. If --F0, --Mdisk0
and --Mdot0 are specified then --Mdot0
is used. Works only when --initialcond
is set to linearF, sinusF or quasistat

--powerorder arg Parameter for the powerlaw initial
condition distribution. This option
works only with --initialcond=powerF or
powerSigma

--gaussmu arg Position of the maximum for Gauss
distribution, positive number not
greater than unity. This option works
only with --initialcond=gaussF

--gausssigma arg Width of for Gauss distribution. This
option works only with
--initialcond=gaussF

--windtype arg (=no) Type of the wind

no: no wind
SS73C: super-Eddington spherical wind
from Shakura-Sunyaev 1973
ShieldsOscil1986: toy wind model from
Shields et al. 1986 which was used to
obtain oscillations in the disk
luminosity. Requires --windC_w and
--windR_w to be specified
Janiuk2015: super-Eddington wind from
Janiuk et al 2015. Requires --windA_0
and --windB_1 to be specified
Shields1986: thermal wind from
Begelman et al. 1983 and Shields et al.
1986. Requires --windXi_max, --windT_ic
and --windPow to be specified
Woods1996AGN: thermal AGN wind from
Woods et al. 1996. Requires --windC_0
and --windT_ic to be specified
Woods1996: thermal wind from Woods et
al. 1996. Requires --windXi_max,
--windT_ic and --windPow to be
specified
toy: a toy wind model used in
arXiv:2105.11974, the mass loss rate is
proportional to the central accretion
rate. Requires --windC_w to be
specified

--windC_w arg The ratio of the mass loss rate due to
wind to the central accretion rate,
|Mwind|/Macc

--windR_w arg The ratio of the wind launch radius to
the outer disk radius, Rwind/Rout

--windA_0 arg Dimensionless parameter characterizing
the strength of the super-Eddington
wind in the framework of the model
Janiuk et al. 2015. Effective value
range from 10 to 25

--windB_1 arg The quantity is of the order of unity.
Characterizes the relationship between
the change in energy per particle and
virial energy.
E = B_1 * k * T

--windXi_max arg Ionization parameter, the ratio of the
radiation and gas pressures

--windT_ic arg Inverse Compton temperature, K.
Characterizes the hardness of the
irradiating spectrum

--windPow arg Multiplicative coefficient to control
wind power

--windC_0 arg Characteristic column density of the
wind mass loss rate from Woods et al.
1996 model, g/(s*cm^2). For AGN approx
value is 3e-13 g/(s*cm^2)

Parameters of accreting neutron star:
:
--nsprop arg (=dummy) Neutron star properties name: defines
geometry (default values of --Rx,
--Risco, and --freqx) and
accretion->radiation efficiency of NS

Values:
dummy: NS accretion->radiation
efficiency is R_g * (1 / R_x - 1 /
2R_in), default --freqx is 0, default
Rx is 1e6, default Risco is Kerr value
newt: NS accretion->radiation
efficiency is a function of NS
frequency, calculated in Newtonian
mechanics (see Lipunova+2021), that's
why --freqx must be specified
explicitly
sibgatullin-sunyaev2000: NS
accretion->radiation efficiency and
default values of Rx and Risco are
functions of NS frequency, calculated
for a specific equation of state for a
NS with weak magnetic field
(Sibgatullin & Sunyaev, 2000, Astronomy
Letters, 26, 699), that's why --freqx
must be specified explicitly

--freqx arg Accretor rotation frequency, Hz. This
parameter is not linked to --kerr,
which could be reconciled manually
(currently, --kerr is not needed for
freddi-ns)

--Rx arg Accretor radius, cm

--Bx arg Accretor polar magnetic induction, G

--hotspotarea arg (=1) Total area of the region on the
accretor radiating because of
accretion, normalized by the accretor
surface area

--epsilonAlfven arg (=1) Magnetosphere radius in units of the
Alfven radius, which is defined as
(mu^4/G/M/sqrt(Mdot))^(1/7)

--inversebeta arg (=0) Not currently in use

--Rdead arg (=0) Maximum inner radius of the disk that
can be achieved, cm

--fptype arg (=no-outflow) Scenario to determine the fraction fp
of accreted mass. The rest of the disk
inner accretion rate is propelled away.

Values:
no-outflow: the matter reaching the
inner disk radius always falls onto NS,
fp = 1
propeller: the matter always flows
away, fp = 0
corotation-block: like 'no-outflow'
when the inner disk radius is smaller
than the corotation radius, like
'propeller' otherwise
geometrical: experimental.
Generalization of 'corotation-block'
for the case of misaligned NS magnetic
axis. Requires --fp-geometrical-chi to
be specified
eksi-kutlu2010: Under construction
romanova2018: fp is an analytical
function of the fastness, found from
MHD simulations by Romanova et al.
(2018, NewA, 62, 94): fp = 1 -
par1*fastness^par2. This requires
--romanova2018-par1 and
--romanova2018-par2 to be specified

--fp-geometrical-chi arg angle between the disk rotation axis
and the NS magnetic axis, used for
--fptype=geometrical, degrees

--romanova2018-par1 arg par1 value for --fptype=romanova2018
and --kappattype=romanova2018

--romanova2018-par2 arg par2 value for --fptype=romanova2018
and --kappattype=romanova2018

--kappattype arg (=const) kappa_t describes how strong is the
interaction between the NS
magnetosphere and disk: total
(accelerating) magnetic torque applied
to the disc is kappa_t(R) * mu^2 / R^3.

Values:
const: doesn't depend on radius,
kappa_t = value. Requires
--kappat-const-value to be specified
corstep: kappa_t can be different
inside and outside the corotation
radius. Requires --kappat-corstep-in
and --kappat-corstep-out to be
specified
romanova2018: experimental. Similar
to corstep option, but the outside
value is reduced by the portion taken
away by the outflow (see Table 2 of
Romanova+2018, NewA, 62, 94). Requires
--kappat-romanova2018-in,
--kappat-romanova2018-out
--romanova2018-par1 and --romanova-par2
to be specified

--kappat-const-value arg (=0.33333333333333331)
kappa_t value for --kappattype=const

--kappat-corstep-in arg (=0.33333333333333331)
kappa_t value inside the corotation
radius for --kappattype=corstep

--kappat-corstep-out arg (=0.33333333333333331)
kappa_t value outside the corotation
radius for --kappattype=corstep

--kappat-romanova2018-in arg (=0.33333333333333331)
kappa_t value inside the corotation
radius for --kappattype=romanova2018

--kappat-romanova2018-out arg (=0.33333333333333331)
kappa_t value outside the corotation
radius for --kappattype=romanova2018

--nsgravredshift arg (=off) Neutron star gravitational redshift
flag.

Values:
off: gravitational redshift is not
taken into account
on: redshift is (1 - R_sch / Rx),
where R_sch = 2GM/c^2

Parameters of self-irradiation:
Qirr = Cirr * (H/r / 0.05)^irrindex * L * psi / (4 pi R^2), where psi is the angular distribution of X-ray radiation
:
--Cirr arg (=0) Irradiation factor for the hot disk

--irrindex arg (=0) Irradiation index for the hot disk

--Cirrcold arg (=0) Irradiation factor for the cold disk

--irrindexcold arg (=0) Irradiation index for the cold disk

--h2rcold arg (=0) Semi-height to radius ratio for the
cold disk

--angulardistdisk arg (=plane) Angular distribution of the disk X-ray
radiation. Values: isotropic, plane

--angulardistns arg (=isotropic) Flag to calculate angular distribution
the NS emission. Values: isotropic,
plane

Parameters of flux calculation:
:
--colourfactor arg (=1.7) Colour factor to calculate X-ray flux

--emin arg (=1) Minimum energy of X-ray band, keV

--emax arg (=12) Maximum energy of X-ray band, keV

--staralbedo arg (=0) Part of X-ray radiation reflected by
optical star, (1 - albedo) heats star's
photosphere. Used only when --starflux
is specified

-i [ --inclination ] arg (=0) Inclination of the system, degrees

--ephemerist0 arg (=0) Ephemeris for the time of the minimum
of the orbital light curve T0, phase
zero corresponds to inferior
conjunction of the optical star, days

--distance arg Distance to the system, kpc

--colddiskflux Add Fnu for cold disk into output file.
Default output is for hot disk only

--starflux Add Fnu for irradiated optical star
into output file. See --Topt, --starlod
and --h2rcold options. Default is
output for the hot disk only

--lambda arg Wavelength to calculate Fnu, Angstrom.
You can use this option multiple times.
For each lambda one additional column
with values of spectral flux density
Fnu [erg/s/cm^2/Hz] is produced

--passband arg Path of a file containing tabulated
passband for a photon counter detector,
the first column for wavelength in
Angstrom, the second column for
transmission factor, columns should be
separated by spaces

Parameters of disk evolution calculation:
:
--inittime arg (=0) Initial time moment, days

-T [ --time ] arg Time interval to calculate evolution,
days

--tau arg Time step, days

--Nx arg (=1000) Size of calculation grid

--gridscale arg (=log) Type of grid for angular momentum h:
log or linear

--starlod arg (=3) Level of detail of the optical star 3-D
model. The optical star is represented
by a triangular tile, the number of
tiles is 20 * 4^starlod

```

**Write which options are mandatory**

Also you can use `freddi.ini` configuration file to store options. This [INI
file](https://en.wikipedia.org/wiki/INI_file) contains lines `option=value`,
option names are the as provided by the help message above. Command line option
overwrites configuration file option. For example, [see
default](https://github.com/hombit/freddi/blob/master/freddi.ini) `freddi.ini`.

Paths where this file is searched are `./freddi.ini` (execution path),
`$HOME/.config/freddi/freddi.ini`, `/usr/local/etc/freddi.ini` and
`/etc/freddi.ini`. You can provide configuration file to Docker container as a
volume: `` -v "`pwd`/freddi.ini":/etc/freddi.ini ``.

#### Output values

`Freddi` outputs time; the accretion rate; the mass of the hot part of the disk;
the outer radius of the hot zone; the irradiation factor; the relative
half-height, effective and irradiation temperature, ratio of the irradiation to
viscous flux at the outer radius of the hot zone; X-ray luminosity (erg/s) in
the band from E\_min to E\_max (`--emin` and `--emax` options); the optical
magnitudes in *U*, *B*, *V*, *R*, *I*, and *J* band ([Allen's Astrophysical
Quantities, Cox 2015](http://www.springer.com/book/9780387951898)); the spectral density flux (erg/s/cm^2/Hz) at some wavelengths set by one or more `--lambda` options.

Snapshot distributions at each time step, if produced, contain the following
data: radial coordinate in terms of the specific angular momentum, radius,
viscous torque, surface density, effective temperature Teff, viscous temperature
Tvis, irradiation temperature Tirr, and the absolute half-height of the disk.