CMR Header

CCMC Metadata Registry (CMR)

Menu Page

Go to:

CMR: View Simulation Run Info

SWMF/20180525/ROR/Motoharu_Nowada_071724_2

Run Description

CCMC ROR run for SWMF 20180525 with RORID Motoharu_Nowada_071724_2

Simulation Time:

Simulation Start Time: 2005-08-24T13:00:00Z
Simulation End Time: 2005-08-24T20:00:00Z
Time Step in second: 60
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 :

Motoharu.Nowada, 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	22.063	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	394848	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	-606.56	-3000	-200
Vy	Plasma velocity in dawn-dusk direction.	The orbital velocity of Earth (about 29 km/s) is usually neglected.	km/s	38.455	-500	500
Vz	Solar wind plasma velocity in north-south direction.		km/s	-102.903	-500	500
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	7	-100	100
By	Dawn-dusk component of solar wind magnetic field.		nT	-20.928	-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	-14.232	-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 Bx value fed into the front boundary of the simulation.		nT	7
By-coefficient	Coefficient for By in linear combination approximating Bx: Bx ~ constant-Bx + By-coefficientBy + Bz-coefficientBz			0	-1	1
Bz-coefficient	Coefficient for Bz in linear combination approximating Bx: Bx ~ constant-Bx + By-coefficientBy + Bz-coefficientBz			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	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'), or use average Bx from solar wind data ('auto').			user
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			2.23
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	25.31	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	-124.22	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	100.7	50	300
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
IE_model	Ionospheric electrodynamics potential solver model name
IE_version	Ionospheric electrodynamics potential solver model version			1.10

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.		high-resolution grid with 9,623,552 cells	overwiew grid with 755136 cells	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.		0.01	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			BATSRUS
GM_version	Global magnetosphere model version			9.30
b_angle	IMF clock angle
GM_dn_init	Number of iteration steps during initialization of the magnetosphere model			2500
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			2005/08/24 13:00
dipole_tilt	Dipole tilt		deg	18.631
dipole_tilt_y	Y component of dipole tilt		deg	-29.8105
corotation	Flag indicating whether to enable corotation around fixed dipole orientation			real
dipole_strength	Dipole strength - fraction of Earth's current magnetic field			1	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	240	60	1800
satellite_output_time_interval	Time interval between outputs during satellite tracking in the magnetosphere (or inner mangetosphere) model.		s	5	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.		cluster1,cluster2,cluster3,cluster4,geotail,goes10,goes11,goes12,goes8,goes9,image,lanl01,lanl02,lanl89,lanl90,lanl94,lanl97,polar		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).			MAG	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	5	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	30	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.		Cluster-1 (FM5/Rumba),Cluster-2 (FM6/Salsa),Cluster-3 (FM7/Samba),Cluster-4 (FM8/Tango),Geotail,GOES-10,GOES-11,GOES-12,GOES-8,GOES-9,IMAGE,LANL-01,LANL-02,LANL-89,LANL-90,LANL-94,LANL-97,Polar		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			RCM
IM_version	Inner magnetosphere model version			2.0
inner_boundary_radius	Inner boundary radius		Re	2.5
inner_boundary_current_radius	Inner boundary current radius		Re	3.0
CPCP-driven_inner_boundary_density	CPCP-driven inner boundary density			1
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.		0.1	0	0.2
density_at_inner_boundary	Density at the inner boundary (1.25 Re)			28	5	500
temperature_at_inner_boundary	Temperature at the inner boundary (1.25 Re)			25000	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

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) :

TPA High AL Substorms

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

spase://CCMC/SimulationModel/SWMF/20180525

List of Publications Referencing this Run :

CMR Footer

Curator: Chiu Wiegand | NASA Official: Dr. Masha Kuznetsova | Privacy and Security Notices | Accessibility | CCMC Data Collection Consent Agreement