Additional optional time-series outputs¶
heat.TAG¶
This files contains informations about the heat transfer (Nusselt number, entropy and
temperature at both boundaries). This file is written by the
subroutine outHeat.
No. of column
Contents
1
time
2
Nusselt number at the inner boundary
3
Nusselt number at the outer boundary
4
Nusselt number based on \(\Delta T\) ratio
5
Temperature at the inner boundary
6
Temperature at the outer boundary
7
Entropy at the inner boundary
8
Entropy at the outer boundary
9
Heat flux at the inner boundary
10
Heat flux at the outer boundary
11
Pressure perturbation at the outer boundary
12
volume integrated mass perturbation
13
Sherwood number at the inner boundary
14
Sherwood number at the outer boundary
15
Sherwood number based on \(\Delta \xi\) ratio
16
Chemical composition at the inner boundary
17
Chemical composition at the outer boundary
This file can be read using MagicTs with the following options:
>>> # To stack all the heat.TAG files of the current directory
>>> ts = MagicTs(field='heat', all=True)
AM.TAG¶
Note
This file is only written when l_AM=.true.
This file contains the time series of the angular momentum of the inner core, the outer
core and the mantle. This file is written by the subroutine write_rot.
No. of column
Contents
1
time
2
angular momentum of the outer core
3
angular momentum of the inner core
4
angular momentum of the mantle
5
total angular momentum
6
relative in angular momentum, per time step
7
total kinetic angular momentum
8
relative change in kinetic energy, per time step
9
kinetic angular momentum of the inner core
10
kinetic angular momentum of the outer core
11
kinetic angular momentum of the mantle
This file can be read using MagicTs with the following options:
>>> # To stack all the AM.TAG files of the current directory
>>> ts = MagicTs(field='AM', all=True)
power.TAG¶
Note
This file is only written when l_power=.true.
This file contains the power budget diagnostic. This file is computed by the subroutine
get_power.
No. of column
Contents
1
time
2
Buoyancy power: \(Ra\,g(r)\,\langle u_r T'\rangle_s\)
3
Chemical power: \(Ra_\xi\,g(r)\,\langle u_r \xi'\rangle_s\)
4
Viscous power at the inner boundary (ICB)
5
Viscous power at the outer boundary (CMB)
6
Viscous dissipation: \(\langle(\nabla \times u)^2\rangle_s\)
7
Ohmic dissipation: \(\langle(\nabla \times B)^2\rangle_s\)
8
Total power at the CMB (viscous + Lorentz)
9
Total power at the ICB (viscous + Lorentz)
10
Total power
11
Time variation of total power
This file can be read using MagicTs with the following options:
>>> # To stack the files that match the pattern ``power.N0m2*``
>>> ts = MagicTs(field='power', tags='N0m2*')
dtE.TAG¶
Note
This file is only written when l_power=.true.
This file contains the time-derivatives of the total energy. It allows to accurately
monitor how the total energy varies with time. This file is generated
by the subroutine output.
No. of column
Contents
1
time
2
time-derivative of the total energy \(\partial E/\partial t\)
3
integrated time variation of the total energy
4
relative time variation of the total energy
earth_like.TAG¶
This contains informations about the Earth-likeness of the CMB radial magnetic
field. This file is written by the subroutine get_e_mag.
Note
This file is only calculated when l_earth_like=.true..
No. of column
Contents
1
time
2
Ratio of axial dipole to non-dipole component at the CMB
3
Equatorial symmetry of the CMB field (odd/even ratio)
4
Zonality: zonal to non-zonal ratio of the CMB field
5
Magnetic flux concentration at the CMB
The details of the calculations are given in (Christensen et al., 2010).
This file can be read using MagicTs with the following options:
>>> # To stack all the earth_like.TAG files of the current directory
>>> ts = MagicTs(field='earth_like', all=True)
geos.TAG¶
This file contains informations about the geostrophy of the flow.
This file is written by the subroutine getEgeos.
Note
This file is only calculated when l_par=.true..
No. of column
Contents
1
time
2
Relative geostrophic kinetic energy
3
Relative kinetic energy in the northern part of the TC
4
Relative kinetic energy in the southern part of the TC
5
Kinetic energy (calculated on the cylindrical grid)
6
North/South correlation of Vz, outside the TC
7
North/South correlation of vorticity outside the TC
8
North/South correlation of helicity outside the TC
9
Geostrophy of axisymmetic flow
10
Geostrophy of zonal flow
11
Geostrophy of meridional flow
12
Geostrophy of non-axisymmetric flow
This file can be read using MagicTs with the following options:
>>> # To stack all the geos.TAG files of the current directory
>>> ts = MagicTs(field='geos', all=True)
helicity.TAG¶
This files contains informations about the kinetic helicity in both the
Northern and the Southern hemispheres. This file is written by the
subroutine outHelicity.
Note
This file is only calculated when l_hel=.true..
No. of column
Contents
1
time
2
Helicity (northern hemisphere)
3
Helicity (southern hemisphere)
4
RMS helicity (northern hemisphere)
5
RMS helicity (southern hemisphere)
6
Helicity (northern hemisphere, only non-axisym. flow)
6
Helicity (southern hemisphere, only non-axisym. flow)
8
RMS helicity (northern hemisphere, only non-axisym. flow)
9
RMS helicity (southern hemisphere, only non-axisym. flow)
This file can be read using MagicTs with the following options:
>>> # To stack all the helicity.TAG files of the current directory
>>> ts = MagicTs(field='helicity', all=True)
u_square.TAG¶
Note
This file is only written in anelastic models, i.e. either when strat/=0 or when interior_model/=”None”
This file contains the square velocity of the outer core. It is actually very similar to the e_kin.TAG file, except that the density background \(\tilde{\rho}\) is removed:
The detailed calculations are done in the subroutine get_u_square. This file contains the following informations:
No. of columns
Contents
1
time
2
poloidal part \({\cal U}_{pol}\)
3
toroidal part \({\cal U}_{pol}\)
4
axisymmetric contribution to the poloidal part
5
axisymmetric contribution to the toroidal part
6
Rossby number: \(Ro=E\,\sqrt{\frac{2{\cal U}}{V}}\)
7
Magnetic Reynolds number: \(Rm=Pm\,\sqrt{\frac{2{\cal U}}{V}}\)
8
local Rossby number: \(Ro_l=Ro\frac{d}{l}\)
9
average flow length scale: \(l\)
10
local Rossby number based on the non-axisymmetric components of the flow
11
average flow length scale based on the non-axisymmetric components of the flow
This file can be read using MagicTs with the following options:
>>> # To stack all the u_square.TAG files of the current directory
>>> ts = MagicTs(field='u_square', all=True)
drift[V|B][D|Q].TAG¶
Note
These files are only written when l_drift=.true.
These files store spherical harmonic coefficients of the toroidal (poloidal) potential of the flow (magnetic) field, only for \(\ell=m\) or \(\ell=m+1\) depending on the symmetry - D for D ipolar and Q for Q uadrupolar. The coefficients are stored at different three different radial levels - n_r1, nr_2, n_r3 for the velocity and two different radial levels - n_r1 and n_r2 - for the magnetic field.
The symmetries can be summarized below:
Field
Dipolar
Quadrupolar
Velocity
\(\ell=m\)
\(\ell=m+1\)
Magnetic
\(\ell=m+1\)
\(\ell=m\)
\(\ell+m=\) even for toroidal potential refers to an equatorially antisymmetric field (Dipolar), while the same for a poloidal potential is associated with an equatorially symmetric field (Quadrupolar). The sense is opposite when \(\ell+m=\) odd. This is the reason for the choice of selecting these specific coefficients.
The columns of the files look like follows:
For the flow field:
Column no.
DriftVD.TAG
DriftVQ.TAG
1
Time
Time
2
\(z\) (minc, minc) at n_r1
\(z\) (minc+1, minc) at n_r1
3
\(z\) (2*minc, 2*minc) at n_r1
\(z\) (2*minc+1, 2*minc) at n_r1
4
\(z\) (3*minc, 3*minc) at n_r1
\(z\) (3*minc+1, 3*minc) at n_r1
5
\(z\) (4*minc, 4*minc) at n_r1
\(z\) (4*minc+1, 4*minc) at n_r1
6
\(z\) (minc, minc) at n_r2
\(z\) (minc+1, minc) at n_r2
7
\(z\) (2*minc, 2*minc) at n_r2
\(z\) (2*minc+1, 2*minc) at n_r2
8
\(z\) (3*minc, 3*minc) at n_r2
\(z\) (3*minc+1, 3*minc) at n_r2
9
\(z\) (4*minc, 4*minc) at n_r2
\(z\) (4*minc+1, 4*minc) at n_r2
10
\(z\) (minc, minc) at n_r3
\(z\) (minc+1, minc) at n_r3
11
\(z\) (2*minc, 2*minc) at n_r3
\(z\) (2*minc+1, 2*minc) at n_r3
12
\(z\) (3*minc, 3*minc) at n_r3
\(z\) (3*minc+1, 3*minc) at n_r3
13
\(z\) (4*minc, 4*minc) at n_r3
\(z\) (4*minc+1, 4*minc) at n_r3
For the magnetic field:
Column no.
DriftBD.TAG
DriftBQ.TAG
1
Time
Time
2
\(b\) (minc+1, minc) at n_r1
\(b\) (minc, minc) at n_r1
3
\(b\) (2*minc+1, 2*minc) at n_r1
\(b\) (2*minc, 2*minc) at n_r1
4
\(b\) (3*minc+1, 3*minc) at n_r1
\(b\) (3*minc, 3*minc) at n_r1
5
\(b\) (4*minc+1, 4*minc) at n_r1
\(b\) (4*minc, 4*minc) at n_r1
6
\(b\) (minc+1, minc) at n_r2
\(b\) (minc, minc) at n_r2
7
\(b\) (2*minc+1, 2*minc) at n_r2
\(b\) (2*minc, 2*minc) at n_r2
8
\(b\) (3*minc+1, 3*minc) at n_r2
\(b\) (3*minc, 3*minc) at n_r2
9
\(b\) (4*minc+1, 4*minc) at n_r2
\(b\) (4*minc, 4*minc) at n_r2
Analysis of these files can give you information about the drift frequency of the solution and it’s symmetry.
iner[P|T].TAG¶
Note
These files are only written when l_iner=.true. and minc = 1.
These files contain time series of spherical harmonic coefficients upto degree,
\(\ell=6\) at a radius \(r = (r_{cmb} - r_{icb})/2\). The inerP.TAG
contains coefficients of the poloidal potential while the inerT.TAG
contains coefficients of the toroidal potential.These files are written by
the subroutine write_rot. The oscillations of these
coefficients can be analysed to look for inertial modes. The
columns of the inerP.TAG look like follows:
No. of column
Coefficient
1
\(w(\ell=1,m=1)\)
2
\(w(\ell=2,m=1)\)
3
\(w(\ell=2,m=2)\)
4
\(w(\ell=3,m=1)\)
…
20
\(w(\ell=6,m=5)\)
21
\(w(\ell=6,m=6)\)
where \(w(\ell,m)\) is the poloidal potential with degree \(\ell\) and order \(m\).
The columns of the inerT.TAG follow the following structure:
No. of column
Coefficient
1
\(z(\ell=1,m=1)\)
2
\(z(\ell=2,m=1)\)
3
\(z(\ell=2,m=2)\)
4
\(z(\ell=3,m=1)\)
…
20
\(z(\ell=6,m=5)\)
21
\(z(\ell=6,m=6)\)
where \(z(\ell,m)\) is the toroidal potential with degree \(\ell\) and order \(m\).
SR[IC|MA].TAG¶
Note
These files are only written for nRotIc=-1 (for SRIC.TAG) or nRotMa=-1 (for SRMA.TAG). In other words, these outputs are produced only when one of the boundaries is made to rotate at a prescribed rotation rate.
These files contain information about power due to torque from viscous and Lorentz forces at the inner core boundary (SRIC.TAG) or core mantle boundary (SRMA.TAG).The columns look like follows:
No. of column
Contents
1
Time
2
\(\Omega_{IC} | \Omega_{MA}\)
3
Total power = Lorentz + Viscous
4
Viscous power
5
Lorentz force power
dtVrms.TAG¶
Note
This file is only written when l_RMS=.true.
This files contains the RMS force balance of the Navier Stokes equation. This file is
written by the subroutine dtVrms.
No. of column
Contents
1
Time
2
Total inertia: dU/dt and advection
3
Coriolis force
4
Lorentz force
5
Advection term
6
Diffusion term
7
Thermal buoyancy term
8
Chemical buoyancy term
9
Pressure gradient term
10
Sum of force terms: geostrophic balance
11
Sum of force terms: pressure, Coriolis and Lorentz
12
Sum of force terms: pressure, buoyancy and Coriolis
13
Sum of force terms: pressure, buoyancy, Coriolis and Lorentz
14
Sum of force terms: Lorentz/Coriolis
15
Sum of force terms: Pressure/Lorentz
16
Sum of force terms: Coriolis/Inertia/Archimedean
This file can be read using MagicTs with the following options:
>>> # To stack all the dtVrms.TAG files of the current directory
>>> ts = MagicTs(field='dtVrms', all=True)
dtBrms.TAG¶
Note
This file is only written when l_RMS=.true.
This files contains the RMS terms that enter the induction equation. This file is
written by the subroutine dtBrms.
No. of column
Contents
1
time
2
Changes in magnetic field (poloidal)
3
Changes in magnetic field (toroidal)
4
Poloidal induction term
5
Toroidal induction term
8
Poloidal diffusion term
9
Toroidal diffusion term
10
Omega effect / toroidal induction term
11
Omega effect
12
Production of the dipole field
13
Production of the axisymmetric dipole field
This file can be read using MagicTs with the following options:
>>> # To stack all the dtBrms.TAG files of the current directory
>>> ts = MagicTs(field='dtBrms', all=True)
perpPar.TAG¶
Note
This file is only written when l_perpPar=.true.
This file contains several time series that decompose the kinetic energy into
components parallel and perpendicular to the rotation axis. This file is
calculated by the subroutine outPerpPar.
No. of column
Contents
1
time
2
Total kinetic energy perpendicular to the rotation axis: \(\frac{1}{2}\langle u_s^2+u_\phi^2 \rangle_V\)
3
Total kinetic energy parallel to the rotation axis: \(\frac{1}{2}\langle u_z^2\rangle_V\)
4
Axisymmetric kinetic energy perpendicular to the rotation axis
5
Axisymmetric kinetic energy parallel to the rotation axis
This file can be read using MagicTs with the following options:
>>> # To stack all the perpPar.TAG files of the current directory
>>> ts = MagicTs(field='perpPar', all=True)
phase.TAG¶
This file contains several diagnostic related to phase field whenever this field is used
by MagIC. This file is calculated by the subroutine
outPhase.
No. of column
Contents
1
time
2
Average radius of the solidus
3
Average temperature at the solidus (should be close to tmelt)
4
Mean spherically-symmetric radius of the solidus
5
Mean spherically-symmetric temperature at the mean spherically symmetric radius of the solidus
6
Minimum radius of the solidus
7
Maximum radius of the solidus
8
Volume of the solid phase
9
Kinetic energy of the solid phase (should be small)
10
Kinetic energy of the liquid phase
11
Heat flux at the outer core boundary
12
Heat flux at the inner core boundary
13
Time variation of of temperature and phase field: \(\frac{\partial}{\partial t}(T-St\Phi)\)
14
Maximum value of phase field (should not exceed one by much, otherwise, Gibbs phenomenon is likely occurring)
15
Minimum value of phase field (should be close to zero, otherwise, Gibbs phenomenon is likely occurring)
>>> # To stack all the phase.TAG files of the current directory >>> ts = MagicTs(field='phase', all=True)
hemi.TAG¶
This file contains diagnostics related to North/South hemisphericity in kinetic and
magnetic energies. This is based on Dietrich and Wicht (2013) work. The file is
calculated by the subroutine outHemi.
No. of column
Contents
1
time
2
relative hemisphericity of \(|u_r|\)
3
relative hemisphericity of kinetic energy
4
relative hemisphericity of \(|B_r|\)
5
relative hemisphericity of magnetic energy
6
relative hemisphericity of \(|B_r|\) at the CMB
7
total kinetic energy (to assess method accuracy)
8
total magnetic energy (to assess method accuracy)
>>> # To stack all the hemi.TAG files of the current directory >>> ts = MagicTs(field='hemi', all=True)
growth_sym.TAG and growth_asym.TAG¶
Those files contain the time series of growth rate of different azimuthal wavenumbers ranging from m_min to m_max. This file is produced when MagIC is used to compute the onset of convection, i.e. when mode=5. growth_sym corresponds to equatorially-symmetric mode, growth_asym to equatorially-asymmetric modes. Those files are produced by the routine get_onset.
No. of column
Contents
1
time
2
growth rate of the azimuthal wave number m_min
3
growth rate of the azimuthal wave number m_min+1
4
growth rate of the azimuthal wave number m_min+2
…
growth rate of the azimuthal wave number m_max
drift_sym.TAG and drift_asym.TAG¶
Those files contain the time series of drift frequency of different azimuthal wavenumbers ranging from m_min to m_max. This file is produced when MagIC is used to compute the onset of convection, i.e. when mode=5. drift_sym corresponds to equatorially-symmetric modes, drift_asym to equatorially-asymmetric modes. Those files are produced by the routine get_onset.
No. of column
Contents
1
time
2
drift frequency of the azimuthal wave number m_min
3
drift frequency of the azimuthal wave number m_min+1
4
drift frequency of the azimuthal wave number m_min+2
…
drift frequency of the azimuthal wave number m_max