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LFM/LTR-2_1_5/ROR/Pavani_Rambachan_092923_1

Run Description

CCMC ROR run for LFM LTR-2_1_5 with RORID Pavani_Rambachan_092923_1

Simulation Time:

Simulation Start Time: 2019-11-27T17:00:00Z
Simulation End Time: 2019-11-27T19:30:00Z
Time Step in second: 120
Simulation Time Description:
Simulation Time Caveats:

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

Regions:

Earth.Magnetosphere
Earth.NearSurface.Ionosphere
Earth.NearSurface.Thermosphere

Simulation Domain :

Contacts :

Pavani.Rambachan, ModelUser

List of Run Input Parameter Grouping and their associated properties :

Name Description Caveats Properties
Settings for the model
Settings used to run the model
Name Description Caveats Units Default Value or Actual Value Valid Min Valid Max
RCM
Inner magnetosphere model options (with RCM or without RCM / CRCM)
run_type
Type of the run - either driven by real data or by artificial conditions
Driven by data
TIEGCM_GPI_file
TIEGCM_GPI_file
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).
True
despike.threshold
De-spike threshold (standard deviations)
sigmas 3 2 4
despike.number_of_samples
De-spike length (number of samples in cluster of extreme values to be eliminated)
5 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') Use average Bx from solar wind data ('auto')
user
b_abs
Magnitude of IMF
3
b_angle
IMF clock angle
-0.96
sw_link
Solar wind link
plot
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
6.87
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.
SW_plot
Name of solar wind plot
Pavani_Rambachan_092923_1_sw.gif
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
2019/11/27 17:00
dipole_tilt
Dipole tilt
deg -11.9368
dipole_tilt_y
Y component of dipole tilt
deg -9.41907
corotation
Flag indicating whether to enable corotation around fixed dipole orientation
real
IE_grid
IE_grid
2x2_44
Run_Ring_Current_Model_or_Not
Flag indicating whether to run Ring Current Model
False
Calculate_Oval_Position_or_Not
Flag indicating whether to run field line tracer to calculate polar cap (region with open field lines).
True
withRCM
Flag indicating whether to use RCM inner magnetosphere model
False
withCIMI
Flag indicating whether to use CIMI inner magnetosphere model
False
withCRCM
Flag indicating whether to use CRCM inner magnetosphere model
False
withRBE
Flag indicating whether to use RBE radiation belt model
False
Provide_Output_Along_Satellite_Trajectory
Flag indicating whether to generate output files along the trajectory of the tracked satellites
False
Provide_CDF_Output_files
Flag indicating whether to provide CDF output files
False
Provide_HDF_Output_files
Flag indicating whether to generate HDF output files
False
Provide_MAGNETOMETER_Output_Files
Flag indicating whether to generate magnetometer output files
False
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
solarwind
Flag indicating whether solar wind data are constant (initial values) or variable (var).
var const var
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
constant-Bx
Constant 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
Bx
Sun-Earth component of solar wind magnetic field.
Bx is usually held constant (zero or average of observed values) to conserve div.B at the front boundary. 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. nT -3.391 -100 100
By
Dawn-dusk component of solar wind magnetic field.
nT -0.05 -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 2.997 -100 100
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 -380.386 -3000 -200
Vy
Plasma velocity in dawn-dusk direction.
The orbital velocity of Earth (about 29 km/s) is usually neglected. km/s 31.241 -500 500
Vz
Solar wind plasma velocity in north-south direction.
km/s 2.873 -500 500
N
Solar wind plasma density.
Mass density described in terms of number of protons per cubic centimeter. AMU/cm^3 3.753 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 48651.5 10000 2000000
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
Ionosphere conductance model
Name Description Caveats Units Default Value or Actual Value Valid Min Valid Max
iono_conductance
Parameter indicationg selection of conductance model in the ionosphere electrodynamics component of the model.
The two models offered for run-on-request are constant (user sets Pedersen Conductance and Hall Conductance) and auroral (conducances driven by f10.7 and field-aligned currents from magnetosphere part of the model). 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
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 69.6 50 300
Magnetosphere model parameters
Name Description Caveats Units Default Value or Actual Value Valid Min Valid Max
inflow boundary
Location of sun-ward facing (front) boundary of the magnetosphere simulation box.
R_E 0 24 128
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. grid with 106x48x64 cells overwiew grid with 755136 cells 1/8 R_E resolution dayside grid with 18,558,976 cells

Run Access Information :

Keyword(s) :

practice

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

spase://CCMC/SimulationModel/LFM/LTR-2_1_5

List of Publications Referencing this Run :

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