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SWIFT
SWIFTsim
Commits
683efd94
Commit
683efd94
authored
Mar 08, 2020
by
Matthieu Schaller
Browse files
Fixed typos and spelling mistakes in the rest of the EAGLE subgrid model description.
parent
971c1ed3
Changes
1
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doc/RTD/source/SubgridModels/EAGLE/index.rst
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683efd94
...
...
@@ -16,7 +16,7 @@ Gas entropy floors
The
gas
particles
in
the
EAGLE
model
are
prevented
from
cooling
below
a
certain
temperature
.
The
temperature
limit
depends
on
the
density
of
the
particles
.
Two
floors
are
used
in
conj
o
nction
.
Both
are
implemented
as
particles
.
Two
floors
are
used
in
conj
u
nction
.
Both
are
implemented
as
polytropic
"equations of states"
:
math
:`
P
=
P_c
\
left
(\
rho
/\
rho_c
\
right
)^\
gamma
`
(
all
done
in
physical
coordinates
),
with
the
constants
derived
from
the
user
input
given
in
terms
of
temperature
and
...
...
@@ -25,10 +25,10 @@ is located in the directory ``src/entropy_floor/EAGLE/`` and the floor
is
applied
in
the
drift
and
kick
operations
of
the
hydro
scheme
.
It
is
also
used
in
some
of
the
other
subgrid
schemes
.
The
first
limit
,
label
l
ed
as
``
Cool
``,
is
typically
used
to
prevent
The
first
limit
,
labeled
as
``
Cool
``,
is
typically
used
to
prevent
low
-
density
high
-
metallicity
particles
to
cool
below
the
warm
phase
because
of
over
-
cooling
induced
by
the
absence
of
metal
diffusion
.
This
limit
plays
only
a
small
role
in
practice
.
The
second
limit
,
label
l
ed
as
``
Jeans
``,
is
only
a
small
role
in
practice
.
The
second
limit
,
labeled
as
``
Jeans
``,
is
used
to
prevent
the
fragmentation
of
high
-
density
gas
into
clumps
that
cannot
be
resolved
by
the
coupled
hydro
+
gravity
solver
.
The
two
limits
are
sketched
on
the
following
figure
.
...
...
@@ -89,7 +89,7 @@ For a normal EAGLE run, that section of the parameter file reads:
SWIFT
will
convert
the
temperature
normalisations
and
Hydrogen
number
density
thresholds
into
internal
energies
and
densities
respectively
assuming
a
neutral
gas
with
primor
i
dal
abundance
pattern
.
This
implies
assuming
a
neutral
gas
with
primord
i
al
abundance
pattern
.
This
implies
that
the
floor
may
not
be
exactly
at
the
position
given
in
the
YAML
file
if
the
gas
has
different
properties
.
This
is
especially
the
case
for
the
temperature
limit
which
will
often
be
lower
than
the
imposed
...
...
@@ -97,7 +97,7 @@ floor by a factor :math:`\frac{\mu_{\rm neutral}}{\mu_{ionised}}
\
approx
\
frac
{
1.22
}{
0.59
}
\
approx
2
`
due
to
the
different
ionisation
states
of
the
gas
.
Recall
that
we
additionally
impose
an
absolute
minium
temperature
at
all
Recall
that
we
additionally
impose
an
absolute
mini
m
um
temperature
at
all
densities
with
a
value
provided
in
the
:
ref
:`
Parameters_SPH
`
section
of
the
parameter
file
.
This
minimal
temperature
is
typically
set
to
100
Kelvin
.
...
...
@@ -197,15 +197,15 @@ In the snapshots, we output for each gas and star particle:
The
stars
will
lose
mass
over
their
lifetime
(
up
to
~
45
%).
The
fractions
will
remain
unchanged
but
if
one
is
interested
in
computing
an
absolute
metal
mass
(
say
)
for
a
star
,
the
``
InitialMass
``
(
see
the
section
(
say
)
for
a
star
,
the
``
InitialMass
es
``
(
see
the
section
:
ref
:`
EAGLE_star_formation
`
below
)
of
the
star
must
be
used
.
The
chemistry
model
only
requires
a
small
number
of
parameters
to
be
specified
in
the
`
EAGLEChemistry
`
section
of
the
YAML
file
.
These
are
the
initial
values
of
the
metallicity
and
element
mass
fractions
.
These
are
then
applied
at
the
start
of
a
simulation
to
*
all
*
the
*
gas
*
particles
.
All
9
traced
elements
have
to
be
specified
An
example
section
,
for
primordial
abundances
(
typical
for
a
cosmological
run
),
is
:
start
of
a
simulation
to
*
all
*
the
gas
and
star
particles
.
All
9
traced
elements
have
to
be
specified
An
example
section
,
for
primordial
abundances
(
typical
for
a
cosmological
run
),
is
:
..
code
::
YAML
...
...
@@ -336,7 +336,7 @@ We note that the EAGLE cooling model does not impose any restriction on the
particles
' individual time-steps. The cooling takes place over the time span
given by the other conditions (e.g the Courant condition).
Fin
e
lly, the cooling module also provides a function to compute the temperature
Fin
a
lly, the cooling module also provides a function to compute the temperature
of a given gas particle based on its density, internal energy, abundances and
the current redshift. This temperature is the one used to compute the cooling
rate from the tables and similarly to the cooling rates, they assume that the
...
...
@@ -366,7 +366,7 @@ and `S`. A valid section of the YAML file looks like:
EAGLECooling:
dir_name: /path/to/the/Wiersma/tables/directory # Absolute or relative path
H_reion_z: 11.5 # Redhift of Hydrogen re-ionization
H_reion_z: 11.5 # Red
s
hift of Hydrogen re-ionization
H_reion_ev_p_H: 2.0 # Energy injected in eV per Hydrogen atom for Hydrogen re-ionization.
He_reion_z_centre: 3.5 # Centre of the Gaussian used for Helium re-ionization
He_reion_z_sigma: 0.5 # Width of the Gaussian used for Helium re-ionization
...
...
@@ -390,7 +390,7 @@ about their evolution. These are updated for a given particle every time it is
active. The EAGLE tracers module is located in the directory
``src/tracers/EAGLE/``.
In the EAGLE model, we trace the maximal tempe
a
rature a particle has reached and
In the EAGLE model, we trace the maximal temperature a particle has reached and
the time at which this happened. When a star is formed (see the section
:ref:`EAGLE_star_formation` below), it inherits all the tracer values of its parent
gas particle. There are no parameters to the model but two values are added to
...
...
@@ -399,7 +399,7 @@ the snapshots for each gas and star particle:
+----------------------------------------+---------------------------------------+-----------+-----------------------------+
| Name | Description | Units | Comments |
+========================================+=======================================+===========+=============================+
| | ``MaximalTemperatures`` | | Mximal temperature reached by
| | [U_T] | |
| | ``MaximalTemperatures`` | | M
a
ximal temperature reached by | | [U_T] | |
| | | this particle. | | |
+----------------------------------------+---------------------------------------+-----------+-----------------------------+
| | ``MaximalTemperaturesScaleFactors`` | | Scale-factor (cosmological runs) | | [-] | |
...
...
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