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SWMF/2023/ROR/CUSTOM-02-GMIE_RLM_042224_3

Run Description

CCMC ROR run for SWMF 2023 with RORID CUSTOM-02-GMIE_RLM_042224_3

Simulation Time:

Simulation Start Time: 2008-03-13T02:00:00Z
Simulation End Time: 2008-03-13T06:00:00Z
Time Step in second: 240
Simulation Time Description:
Simulation Time Caveats:

Temporal Dependence (whether the outputs of the simulation code are time-dependent?): true

Regions:

Earth.Magnetosphere
Earth.Magnetosphere.Magnetotail
Earth.Magnetosphere.Main
Earth.Magnetosphere.RadiationBelt
Earth.NearSurface.AuroralRegion
Earth.NearSurface.PolarCap

Simulation Domain :

Coordinate System:
    Coordinate Representation:Cartesian CoordinateSystemName: GSM
Simulation Domain Description: Rectangular box containing magnetosphere.
Simulation Domain Caveats: Near-Earth boundary above ionosphere and current layer.
Spatial Dimension: 3
Velocity Dimension: 1
Field Dimension: 1
Units: R_E
Coordinates Label: X, Y, Z
Valid Min: -1000
Valid Max: 1000
Grid Structure: Block-adaptive octree.
Grid Cell Size: 0.0
Symmetry: None
Boundary Condition:
    Boundary Type: FieldBoundary
    Front Wall: inflow
    Back Wall: outflow
    Side Wall: outflow
    Obstacle: no flow

Contacts :

Mostafa.El-Alaoui, ModelUser

List of Run Input Parameter Grouping and their associated properties :

Name Description Caveats Properties
Solar wind inputs
Time-dependent solar wind plasma and magnetic field inputs.
Solar wind inputs are derived from a single spacecraft usually 200 R_E upstream of the sun-ward (front) simulation box boundary.
Name Description Caveats Units Default Value or Actual Value Valid Min Valid Max
N
Solar wind plasma density.
Mass density described in terms of number of protons per cubic centimeter. AMU/cm^3 2.427 0.1 100
T
Solar wind plasma temperature.
Derived from observed distribution of solar wind particles. Can fluctuate widely when density N is at or below 1 AMU/cm^3. K 162728 10000 2000000
Vx
Sun-Earth component of solar wind velocity.
Low solar wind speed (less than 200 km/s in magnitude) usually indicates poor statistics in the solar wind plasma measurements. km/s -627.666 -3000 -200
Vy
Plasma velocity in dawn-dusk direction.
The orbital velocity of Earth (about 29 km/s) is usually neglected. km/s 14.005 -500 500
Vz
Solar wind plasma velocity in north-south direction.
km/s 8.491 -500 500
Bx
Sun-Earth component of solar wind magnetic field.
(1) Bx is usually held constant (zero or average of observed values) to conserve div.B at the front boundary. (2) time dependent Bx. (3) Alternatively, oblique phase fronts can be assumed that update solar wind conditions along those fronts throughout the front boundary. Bx is then approximated as a linear combination of time dependent By and Bz. time dependent Bx nT -3.381 -100 100
By
Dawn-dusk component of solar wind magnetic field.
nT -0.494 -100 100
Bz
North-south component of the solar wind magnetic field. 
B_z is most important magnetic field component to drive or inhibit geomagnetic activity.
Other components play a role in connection with the orientation of the Earth's dipole field.
nT -0.43 -100 100
sw_source
Name of the spacecraft or data source used to generate solar wind input information.
Currently one of ACE-RT ACE-L2, WIND, OMNI, DSCOVR (real time)
User-submitted data may be from any source or made-up. OMNI
solarwind
Flag indicating whether solar wind data are constant (initial values) or variable (var).
var const var
constant-Bx
Constant or time dependent Bx value fed into the front boundary of the simulation.
nT 0
By-coefficient
Coefficient for By in linear combination approximating Bx: 
Bx ~ constant-Bx + By-coefficient*By + Bz-coefficient*Bz
0 -1 1
Bz-coefficient
Coefficient for Bz in linear combination approximating Bx: Bx ~ constant-Bx + By-coefficient*By + Bz-coefficient*Bz
0 -1 1
SW density floor
Lowest value of N applied during pre-processing of solar wind input data.
The density floor in the solar wind varies by magnetosphere model and it's numerical stability. A similar floor may be imposed inside the magnetotail lobes where the density may drop lower than in the solar wind. AMU/cm^3 0.1 0.1 2.5
despike_solar_wind_data
Flag indicating whether to automatically de-spike solar wind (optional for automatically retrieved data only; use when solar wind data shown in next page have clusters of extreme values in plasma density, temperature or velocity).
Despiking is performed during preprocessing of solar wind inputs. The option is available during run -on request submission on the CCMC web site. True 0 1
despike.threshold
De-spike threshold (standard deviations)
sigmas 2 2 4
despike.number_of_samples
De-spike length (number of samples in cluster of extreme values to be eliminated)
3 3 9
setting_option_for_Bx
Indicates how solar wind Bx is set: set Bx to a specified constant ('user'), set Bx to the initial solar wind data value ('init'), or use average Bx from solar wind data ('auto').
observed
SW_density_floor_was_applied
Flag indicating the solar wind density has been floored with SW_density_floor value to ensure that the model will run through the requested time interval.
False
minimum_SW_Fast-Mode_mach_number
Minimum solar wind Fast-Mode mach number
7.54
SW_parameters_are_large
Flag indicating whether solar wind velocity, density or dynamic pressure are large. If they are, the run is a special request requiring attention by CCMC staff. The variables will be accepted unless they exceed certain absolute maximum values.
b_abs
Magnitude of transverse solar wind magnetic field b_abs=sqrt(B_y^2 + B_z^2)
nT 0.65 0 100 (100000 for EXO)
b_angle
Clock angle of transverse solar wind magnetic field orientation, measured from northward direction. b_angle=atan(B_y,B_z) cast into range from 0 to 360 degrees.
degree -131.04 0 360
Ionosphere conductance model
Name Description Caveats Units Default Value or Actual Value Valid Min Valid Max
f10.7
Solar irradiation index as represented by the flux of 10.7 cm (2800 MHz) radiation from the Sun measured in units of 10−22 W⋅m−2⋅Hz−1. 
Daily index of solar radiation that affects the daytime background conductivity in the ionosphere. sfu 68.7 50 300
iono_conductance
Parameter indicationg selection of conductance model in the ionosphere electrodynamics component of the model.
The IE model uses the Ridley Legacy Model (RLM) with a constant conductance plus one of these additions: 1. Conductance Model for Extreme Events (CMEE), 2. COnductance Model based on PFISR And the SWARM Satellite (COMPASS), 3. Asymmetric Pedersen Conductance (ASYM), and 4. AMPERE-Derived Electrodynamic Parameters of the High Latitude Ionosphere (ADELPHI). auroral constant auroral
Pedersen Conductance
Value of constant user-selected Pedersen Conductance in the ionosphere.
S 1 100
Hall Conductance
Value of constant user-selected Hall Conductance in the ionosphere.
S 0 100
IE_model
Ionospheric electrodynamics potential solver model name
IE_version
Ionospheric electrodynamics potential solver model version
Magnetosphere model parameters
Name Description Caveats Units Default Value or Actual Value Valid Min Valid Max
grid
Grid definition referred to by number of cells.
The grids for the different global magnetosphere models are listed in a file GM_grids.txt.
The design of SWMF grids is limitless and cannot be represented adequately with a single parameter. 1,905,904 cells, 1/8 resolution at inner boundary overwiew grid with 1,905,904cells 1/8 R_E resolution dayside grid with 18,558,976 cells
GM_boris_clight_factor
The Boris factor reduces the speed of light in a MHD equations, thus reducing the numerical stiffness and allowing explicit time steps to be longer.
The light speed is the largest wave speed in the numerical system. Wave phenomena might be lost with a light speed that is too low. 0.02 0.005 1.0
GM_resistivity_model
Type of magnetosphere resistivity model applied. This can be anomalous resistivity driven by electric currents, constant resistivity or hyper-diffusion (artificial resistivity triggered by grid-scale gradients).
A non-zero resistivity is applied only outside of 2 near-Earth boundary radii. none
GM_resistivity_value
Value of constant resistivity in magnetosphere.
m^2/s 0 0 1.0E13
GM_anomalous_resistivity_value
Resisitivty factor in anomalous 9current-driven)resistivity model.
resistivity = GM_resistivity_value + GM_anomalous_resistivity_value*(J-GM_resistivity_current_threshold)^2
m^2/s 0 0 1e15
GM_resistivity_current_threshold
Current value above which anomalous resistivity begins.
muA/m^2 0.7 0 10
GM_anomalous_resistivity_max_value
Maximum value attained by anomalous resistivity model. Resistivity in thin current sheets with large current densities cannot exceed this value.
m^2/s 0 0 1e15
inflow boundary
Location of sun-ward facing (front) boundary of the magnetosphere simulation box.
R_E 32 24 128
GM_model
Global magnetosphere model name
GM_version
Global magnetosphere model version
b_angle
IMF clock angle
GM_dn_init
Number of iteration steps during initialization of the magnetosphere model
GM_solver
Numerical solver for magnetosphere MHD
Rusanov
GM_limiter_name
Limiter name for magnetosphere MHD
mc3
GM_limiter_beta
Limiter beta
1
GM_implicit
Time advance mode in magnetosphere
explicit
GM_timestep
Magnetosphere time step (for part-implicit advance only)
dipole_update
Flag indicating whether dipole updates throughout the run (True) or dipole set to start time of run (False)
True
dipole_time
Dipole time
2008/03/13 02:00
dipole_tilt
Dipole tilt
deg -11.5448
dipole_tilt_y
Y component of dipole tilt
deg 30.4237
corotation
Flag indicating whether to enable corotation around fixed dipole orientation
real
dipole_strength
Dipole strength - fraction of Earth's current magnetic field
0.05 1
Model outputs
Parameters that define the type of outputs generated and the frequency of outputs.
Name Description Caveats Units Default Value or Actual Value Valid Min Valid Max
output_time_interval
Time interval between outputs in the magnetosphere and ionosphere electrodynamics.
Other components within a global magnetosphere modeling framework such as ring current or thermosphere model may have their own time scales. Output cadences may differ. s 60 60 1800
satellite_output_time_interval
Time interval between outputs during satellite tracking in the magnetosphere (or inner mangetosphere) model.
s 60 1 60
SSCWeb_satellite_names
Comma-separated list of satellite names (single-word strings used in SSCweb).
Satellite trajectories are obtained from SSCweb's Locator Tabular interface and are typically limited to missions in geospace. themisa,themisb,themisc,themisd,themise all satellites in SSCweb that are aloft at any time during a model run's time interval
MAGNETOMETERGRID
Flag indicating the use of the SWMF model's calculation of ground magnetic perturbations on a grid of positions.
Magnetic perturbations on the ground are calculated using Biot-Savart summation over electric currents on the magnetosphere and ionosphere electrodynamics grids. magnetic-field=aligned currents between ionosphere electrodynamics and magnetosphere are assumed to flow on dipole magnetic field lines. The calculation assumes stationary conditions (infinite speed of light) and does not take into account induction effects due to the Earth's electric ground conductivity. True false true
coord_MAGNETOMETERGRID
Coordinate system used in the grid of positions on the ground.
This is either GEO (geographic) or MAG (geomagnetic).
GEO GEO MAG
latmin_MAGNETOMETERGRID
Minimum latitude of the position grid used to calculate ground magnetic perturbations.
degrees -90 -90 90
latmax_MAGNETOMETERGRID
Maximum latitude of the position grid used to calculate ground magnetic perturbations.
degrees 90 -90 90
lonmin_MAGNETOMETERGRID
Minimum longitude of grid used to calculate ground magnetic perturbations.
degrees 0 0 360
lonmax_MAGNETOMETERGRID
Maximum longitude of grid used to calculate ground magnetic perturbations.
degrees 360 0 360
dlat_MAGNETOMETERGRID
Latitude spacing in grid used to calculate ground magnetic perturbations.
degrees 2 1 180
dlon_MAGNETOMETERGRID
Longitude spacing in grid used to calculate ground magnetic perturbations.
degrees 5 1 360
dtsave_MAGNETOMETERGRID
Time interval between calculation and output of ground magnetic perturbations.
s 5 300
satellite_names
Comma-separated list of satellite names
Satellite trajectories are obtained from SSCweb's Locator Tabular interface and are typically limited to missions in geospace. THEMIS-A (P5),THEMIS-B (P1),THEMIS-C (P2),THEMIS-D (P3),THEMIS-E (P4) all satellites in SSCweb that are aloft at any time during a model run's time interval
Provide_Output_Along_Satellite_Trajectory
Flag indicating whether to generate output files along the trajectory of the tracked satellites
True
dnsave_MAGNETOMETERGRID
Number of steps between outputs when calculating magnetic perturbations on grid of locations
Currently unused -1
Provide_CDF_Output_files
Flag indicating whether to provide CDF output files
This is a post-processing option within the CCMC run-on-request workflow. The option does not affect how the model itself runs. False
Provide_HDF_Output_files
Flag indicating whether to generate HDF output files
This is a post-processing option within the CCMC run-on-request workflow. The option does not affect how the model itself runs. False
Provide_MAGNETOMETER_Output_Files
Flag indicating whether to generate magnetometer output files
True
Calculate_Oval_Position_or_Not
Flag indicating whether to run field line tracer to calculate polar cap (region with open field lines).
This is a post-processing option within the CCMC run-on-request workflow. The option does not affect how the model itself runs. True
Exoplanetary run parameters
Parameters pertaining to an exoplanetary run
Name Description Caveats Units Default Value or Actual Value Valid Min Valid Max
EXO
Flag indicating whether this is an exoplanetary run
0
Inner magnetosphere model parameters
Name Description Caveats Units Default Value or Actual Value Valid Min Valid Max
IM_model
Inner magnetosphere model name
IM_version
Inner magnetosphere model version
inner_boundary_radius
Inner boundary radius
Re
inner_boundary_current_radius
Inner boundary current radius
Re
CPCP-driven_inner_boundary_density
CPCP-driven inner boundary density
0
factor_for_CPCP-driven_inner_boundary_density
Factor for CPCP-driven inner boundary density.
Inner Boundary Density=CPCP-driven_inner_boundary_density + CPCP*factor_for_CPCP-driven_inner_boundary_density
with CPCP the Cross-PolarCap Potential (in kV) - the maximum electric potential minus the minimum potential in the ionosphere electrodynamics (IE) solver.
The maximum value is unknown. A value of 0.1 was recommended by the modelers. Larger values may work but may overly dampen storm time acitivity. 0 0 0.2
density_at_inner_boundary
Density at the inner boundary (1.25 Re)
5 500
temperature_at_inner_boundary
Temperature at the inner boundary (1.25 Re)
1500 5000
Radiation belt model
Name Description Caveats Units Default Value or Actual Value Valid Min Valid Max
RB_model
Radiation belt model name
RB_version
Radiation belt model version
General parameters
Name Description Caveats Units Default Value or Actual Value Valid Min Valid Max
run_type
Type of the run - either driven by real data or by artificial conditions
Driven by data
preset
The name of the preset used for the run
Custom
Ring current model
Name Description Caveats Units Default Value or Actual Value Valid Min Valid Max
Run_Ring_Current_Model_or_Not
Flag indicating whether to run Ring Current Model
This is a post-processing option within the CCMC run-on-request workflow. The option does not affect how the model itself runs. False

Run Access Information :

Keyword(s) :

Test custom run Ridley

Linked to Parent Spase Resource(s) (example: SimulationModel) :

spase://CCMC/SimulationModel/SWMF/2023

List of Publications Referencing this Run :

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