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StrongGravity
KYNreverb
Commits
cea7a934
Commit
cea7a934
authored
Sep 20, 2018
by
Michal Dovčiak
Browse files
Small corrections in documentation.
parent
121bdf73
Changes
4
Hide whitespace changes
Inline
Side-by-side
README.md
View file @
cea7a934
...
...
@@ -177,16 +177,16 @@ source code. Summary of the parameters:
*
**par2 ... theta_o**
-
observer inclination in degrees (0
°
-pole, 90
°
-disc)
*
**par3 ... rin**
-
inner edge of non-zero disc emissivity (in GM/c^2 or in r
~mso~
)
-
inner edge of non-zero disc emissivity (in GM/c^2 or in r
<sub>
mso
</sub>
)
*
**par4 ... ms**
-
switch for inner edge
-
0: we integrate from inner edge = par3
-
1: if the inner edge of the disc is below marginally stable orbit (MSO)
then we integrate emission above MSO only
-
2: we integrate from inner edge given in units of MSO, i.e. inner
edge = par3
×
r
~mso~
(the same applies for outer edge)
edge = par3
×
r
<sub>
mso
</sub>
(the same applies for outer edge)
*
**par5 ... rout**
-
outer edge of non-zero disc emissivity (in GM/c^2 or in r
~mso~
)
-
outer edge of non-zero disc emissivity (in GM/c^2 or in r
<sub>
mso
</sub>
)
*
**par6 ... phi**
-
lower azimuth of non-zero disc emissivity (degrees)
*
**par7 ... dphi**
...
...
@@ -199,17 +199,17 @@ source code. Summary of the parameters:
source is located (GM/c^(2))
*
**par10 ... PhoIndex**
-
power-law energy index of the primary flux
*
**par11 ... L/L
~Edd~
**
*
**par11 ... L/L
<sub>Edd</sub>
**
-
dE/dt, the intrinsic local (if negative) or the observed
(if positive) primary isotropic flux in the X-ray energy range 2-10keV
in units of L
~Edd~
in units of L
<sub>
Edd
</sub>
*
**par12 ... Np:Nr**
-
ratio of the primary to the reflected normalization
-
1: self-consistent model for isotropic primary source
-
0: only reflection, primary source is hidden
-
if positive then L/L
~Edd~
(par11) means the luminosity towards the
-
if positive then L/L
<sub>
Edd
</sub>
(par11) means the luminosity towards the
observer
-
if negative then L/L
~Edd~
(par11) means the luminosity towards the disc
-
if negative then L/L
<sub>
Edd
</sub>
(par11) means the luminosity towards the disc
*
**par13 ... density/ionisation**
-
density profile normalization in 10^15 cm^(-3) if positive
-
ionisation profile normalisation if it is negative
...
...
@@ -230,7 +230,7 @@ source code. Summary of the parameters:
-
abs(par16) > 1: the fraction of thermalisation is computed from
difference between the incident and reflected fluxes
*
**par17 ... arate**
-
accretion rate in units of L
~Edd~
if positive or in Solar mass per
-
accretion rate in units of L
<sub>
Edd
</sub>
if positive or in Solar mass per
Julian year (365.25 days) if negative
*
**par18 ... f_col**
-
spectral hardening factor
...
...
@@ -330,8 +330,8 @@ source code. Summary of the parameters:
Af
×
f^(qf), used for par38=+16 and par38=+18;
if par36=-1 then the following hard lags prescription is used (see
Epitropakis & Papadakis, 2017):
100
* log10(E
~ref~
/E) *
(f/1e-4)^(-1) s
with E
~ref~
being middle of the reference energy band and E middle of
100
* log10(E
<sub>ref</sub>
/E) *
(f/1e-4)^(-1) s
with E
<sub>
ref
</sub>
being middle of the reference energy band and E middle of
the energy band of interest
*
**par37 ... Amp/qf**
-
multiplicative factor for the amplitude-energy dependence in case of
...
...
@@ -527,16 +527,16 @@ source code. Summary of the parameters:
*
**par2 ... theta_o**
-
observer inclination in degrees (0
°
-pole, 90
°
-disc)
*
**par3 ... rin**
-
inner edge of non-zero disc emissivity (in GM/c^2 or in r
~mso~
)
-
inner edge of non-zero disc emissivity (in GM/c^2 or in r
<sub>
mso
</sub>
)
*
**par4 ... ms**
-
switch for inner edge
-
0: we integrate from inner edge = par3
-
1: if the inner edge of the disc is below marginally stable orbit (MSO)
then we integrate emission above MSO only
-
2: we integrate from inner edge given in units of MSO, i.e. inner
edge = par3
×
r
~mso~
(the same applies for outer edge)
edge = par3
×
r
<sub>
mso
</sub>
(the same applies for outer edge)
*
**par5 ... rout**
-
outer edge of non-zero disc emissivity (in GM/c^2 or in r
~mso~
)
-
outer edge of non-zero disc emissivity (in GM/c^2 or in r
<sub>
mso
</sub>
)
*
**par6 ... phi**
-
lower azimuth of non-zero disc emissivity (degrees)
*
**par7 ... dphi**
...
...
@@ -549,17 +549,17 @@ source code. Summary of the parameters:
source is located (GM/c^(2))
*
**par10 ... PhoIndex**
-
power-law energy index of the primary flux
*
**par11 ... L/L
~Edd~
**
*
**par11 ... L/L
<sub>Edd</sub>
**
-
dE/dt, the intrinsic local (if negative) or the observed
(if positive) primary isotropic flux in the X-ray energy range 2-10keV
in units of L
~Edd~
in units of L
<sub>
Edd
</sub>
*
**par12 ... Np:Nr**
-
ratio of the primary to the reflected normalization
-
1: self-consistent model for isotropic primary source
-
0: only reflection, primary source is hidden
-
if positive then L/L
~Edd~
(par11) means the luminosity towards the
-
if positive then L/L
<sub>
Edd
</sub>
(par11) means the luminosity towards the
observer
-
if negative then L/L
~Edd~
(par11) means the luminosity towards the disc
-
if negative then L/L
<sub>
Edd
</sub>
(par11) means the luminosity towards the disc
*
**par13 ... density/ionisation**
-
density profile normalization in 10^15 cm^(-3) if positive,
i.e. n = par13
×
r^(par14)
...
...
@@ -588,7 +588,7 @@ source code. Summary of the parameters:
-
abs(par17) > 1: the fraction of thermalisation is computed from
difference between the incident and reflected fluxes
*
**par18 ... arate**
-
accretion rate in units of L
~Edd~
if positive or in Solar mass per
-
accretion rate in units of L
<sub>
Edd
</sub>
if positive or in Solar mass per
Julian year (365.25 days) if negative
*
**par19 ... f_col**
-
spectral hardening factor
...
...
@@ -695,8 +695,8 @@ source code. Summary of the parameters:
Af
×
f^(qf), used for par38=+16 and par38=+18;
if par36=-1 then the following hard lags prescription is used (see
Epitropakis & Papadakis, 2017):
100
* log10(E
~ref~
/E) *
(f/1e-4)^(-1) s
with E
~ref~
being middle of the reference energy band and E middle of
100
* log10(E
<sub>ref</sub>
/E) *
(f/1e-4)^(-1) s
with E
<sub>
ref
</sub>
being middle of the reference energy band and E middle of
the energy band of interest
*
**par37 ... Amp/qf**
-
multiplicative factor for the amplitude-energy dependence in case of
...
...
lmodel-kynreverb.dat
View file @
cea7a934
...
...
@@ -26,7 +26,7 @@ $tab 2.
$sw 1.
ntable " " 80. 0. 0. 99. 99. -1.
nrad " " -4488. -10000. -10000. 10000. 10000. -100.
division " " -1.
0
.
0
. 1. 1. -1.
division " " -1.
-1
.
-1
. 1. 1. -1.
nphi " " 180. 1. 1. 20000. 20000. -100.
deltaT GM/c^3 1. 1e-3 1e-3 10. 10. -0.05
nt_ratio " " 1. 1. 1. 10. 10. -1.
...
...
@@ -67,7 +67,7 @@ limb " " 0. 0. 0. 2. 2. -1.
$tab 11.
ntable " " 80. 0. 0. 99. 99. -1.
nrad " " -4488. -10000. -10000. 10000. 10000. -100.
division " " -1.
0
.
0
. 1. 1. -1.
division " " -1.
-1
.
-1
. 1. 1. -1.
nphi " " 180. 1. 1. 20000. 20000. -100.
deltaT GM/c^3 1. 1e-3 1e-3 10. 10. -0.05
nt_ratio " " 1. 1. 1. 10. 10. -1.
...
...
xskynrefrev.c
View file @
cea7a934
...
...
@@ -457,8 +457,8 @@ param[ 8] = 3.; // height
param
[
9
]
=
2
.;
// PhoIndex
param
[
10
]
=
0
.
001
;
// L/Ledd
param
[
11
]
=
1
.;
// Np:Nr
param
[
12
]
=
1
.;
// density
param
[
13
]
=
0
.;
// den_prof
param
[
12
]
=
1
.;
// density
/ionisation
param
[
13
]
=
0
.;
// den_prof
/ion_prof
param
[
14
]
=
1
.;
// abun
param
[
15
]
=
0
.;
// thermalisation
param
[
16
]
=
0
.
1
;
// arate
...
...
@@ -2060,8 +2060,8 @@ for(ie=0;ie<ne;ie++){
spectrum
[
ie
]
=
0
.;
for
(
it
=
0
;
it
<
nt
;
it
++
)
spectrum
[
ie
]
+=
far
[
ie
+
ne
*
it
];
// we have to divide by duration of the flare, flare_duration_rg, however,
// we did not multiply by deltaT, thus we have to
divide by
// flare_duration_rg / (deltaT)
// we did not multiply by deltaT
(i.e. far is per second)
, thus we have to
//
divide by
flare_duration_rg / (deltaT)
spectrum
[
ie
]
*=
dt
/
flare_duration_rg
;
if
(
NpNr
!=
0
.)
spectrum_prim
[
ie
]
=
far_prim
[
ie
];
}
...
...
@@ -2268,6 +2268,7 @@ if(photar_sw){
// photar[ie] /= flare_duration_rg; <-- we have already divided by flare duration!
}
}
else
if
(
time1
>=
time2
){
// we compute flux per second at time time1
// given time1, find the corresponding index in time[]:
it0
=
(
int
)
ceil
(
(
time1
-
time
[
0
])
/
deltaT
+
1
);
if
(
it0
<
1
)
it0
=
1
;
...
...
@@ -2310,7 +2311,10 @@ if(photar_sw){
// all the whole bins
for
(
it
=
it0
+
1
;
it
<
itn
;
it
++
)
photar
[
ie
]
+=
(
far
[
ie
+
ne
*
it
]
+
far
[
ie
+
ne
*
(
it
-
1
)])
/
2
.;
photar
[
ie
]
*=
dt
/
flare_duration_rg
;
if
(
NpNr
!=
0
.)
photar
[
ie
]
+=
far_prim
[
ie
];
if
(
NpNr
!=
0
.
&&
time1_rg
<=
flare_duration_rg
){
if
(
time2_rg
<
flare_duration_rg
)
photar
[
ie
]
+=
far_prim
[
ie
]
*
(
time2
-
time1
);
else
photar
[
ie
]
+=
far_prim
[
ie
]
*
(
flare_duration_sec
-
time1
);
}
}
}
}
...
...
xskynxilrev.c
View file @
cea7a934
...
...
@@ -475,8 +475,8 @@ param[ 8] = 3.; // height
param
[
9
]
=
2
.;
// PhoIndex
param
[
10
]
=
0
.
001
;
// L/Ledd
param
[
11
]
=
1
.;
// Np:Nr
param
[
12
]
=
1
.;
// density
param
[
13
]
=
0
.;
// den_prof
param
[
12
]
=
1
.;
// density
/ionisation
param
[
13
]
=
0
.;
// den_prof
/ion_prof/density
param
[
14
]
=
1
.;
// abun
param
[
15
]
=
300
.;
// E_cut
param
[
16
]
=
0
.;
// thermalisation
...
...
@@ -3064,8 +3064,8 @@ for(ie=0;ie<ne;ie++){
spectrum
[
ie
]
=
0
.;
for
(
it
=
0
;
it
<
nt
;
it
++
)
spectrum
[
ie
]
+=
far
[
ie
+
ne
*
it
];
// we have to divide by duration of the flare, flare_duration_rg, however,
// we did not multiply by deltaT, thus we have to
divide by
// flare_duration_rg / (deltaT)
// we did not multiply by deltaT
(i.e. far is per second)
, thus we have to
//
divide by
flare_duration_rg / (deltaT)
spectrum
[
ie
]
*=
dt
/
flare_duration_rg
;
if
(
NpNr
!=
0
.)
spectrum_prim
[
ie
]
=
far_prim
[
ie
];
}
...
...
@@ -3272,6 +3272,7 @@ if(photar_sw){
// photar[ie] /= flare_duration_rg; <-- we have already divided by flare duration!
}
}
else
if
(
time1
>=
time2
){
// we compute flux per second at time time1
// given time1, find the corresponding index in time[]:
it0
=
(
int
)
ceil
(
(
time1
-
time
[
0
])
/
deltaT
+
1
);
if
(
it0
<
1
)
it0
=
1
;
...
...
@@ -3314,7 +3315,10 @@ if(photar_sw){
// all the whole bins
for
(
it
=
it0
+
1
;
it
<
itn
;
it
++
)
photar
[
ie
]
+=
(
far
[
ie
+
ne
*
it
]
+
far
[
ie
+
ne
*
(
it
-
1
)])
/
2
.;
photar
[
ie
]
*=
dt
/
flare_duration_rg
;
if
(
NpNr
!=
0
.)
photar
[
ie
]
+=
far_prim
[
ie
];
if
(
NpNr
!=
0
.
&&
time1_rg
<=
flare_duration_rg
){
if
(
time2_rg
<
flare_duration_rg
)
photar
[
ie
]
+=
far_prim
[
ie
]
*
(
time2
-
time1
);
else
photar
[
ie
]
+=
far_prim
[
ie
]
*
(
flare_duration_sec
-
time1
);
}
}
}
}
...
...
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