CCMC Metadata Registry (CMR)

Solar wind plasma density.

Solar wind plasma temperature.

Sun-Earth component of solar wind velocity.

Plasma velocity in dawn-dusk direction.

Solar wind plasma velocity in north-south direction.

Sun-Earth component of solar wind magnetic field.

Dawn-dusk component of solar wind magnetic field.

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.

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)

Flag indicating whether solar wind data are constant (initial values) or variable (var).

Constant or time dependent Bx value fed into the front boundary of the simulation.

Coefficient for By in linear combination approximating Bx: 
Bx ~ constant-Bx + By-coefficient*By + Bz-coefficient*Bz

Coefficient for Bz in linear combination approximating Bx: Bx ~ constant-Bx + By-coefficient*By + Bz-coefficient*Bz

Lowest value of N applied during pre-processing of solar wind input 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).

De-spike threshold (standard deviations)

De-spike length (number of samples in cluster of extreme values to be eliminated)

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').

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.

Minimum solar wind Fast-Mode mach number

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.

Magnitude of transverse solar wind magnetic field b_abs=sqrt(B_y^2 + B_z^2)

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.

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. 

Parameter indicationg selection of conductance model in the ionosphere electrodynamics component of the model.

Value of constant user-selected Pedersen Conductance in the ionosphere.

Value of constant user-selected Hall Conductance in the ionosphere.

Ionospheric electrodynamics potential solver model name

Ionospheric electrodynamics potential solver model version

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 Boris factor reduces the speed of light in a MHD equations, thus reducing the numerical stiffness and allowing explicit time steps to be longer.

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).

Value of constant resistivity in magnetosphere.

Resisitivty factor in anomalous 9current-driven)resistivity model.
resistivity = GM_resistivity_value + GM_anomalous_resistivity_value*(J-GM_resistivity_current_threshold)^2

Current value above which anomalous resistivity begins.

Maximum value attained by anomalous resistivity model. Resistivity in thin current sheets with large current densities cannot exceed this value.

Location of sun-ward facing (front) boundary of the magnetosphere simulation box.

Global magnetosphere model name

Global magnetosphere model version

IMF clock angle

Number of iteration steps during initialization of the magnetosphere model

Numerical solver for magnetosphere MHD

Limiter name for magnetosphere MHD

Limiter beta

Time advance mode in magnetosphere

Magnetosphere time step (for part-implicit advance only)

Flag indicating whether dipole updates throughout the run (True) or dipole set to start time of run (False)

Dipole time

Dipole tilt

Y component of dipole tilt

Flag indicating whether to enable corotation around fixed dipole orientation

Dipole strength - fraction of Earth's current magnetic field

Time interval between outputs in the magnetosphere and ionosphere electrodynamics.

Time interval between outputs during satellite tracking in the magnetosphere (or inner mangetosphere) model.

Comma-separated list of satellite names (single-word strings used in SSCweb).

Flag indicating the use of the SWMF model's calculation of ground magnetic perturbations on a grid of positions.

Coordinate system used in the grid of positions on the ground.
This is either GEO (geographic) or MAG (geomagnetic).

Minimum latitude of the position grid used to calculate ground magnetic perturbations.

Maximum latitude of the position grid used to calculate ground magnetic perturbations.

Minimum longitude of grid used to calculate ground magnetic perturbations.

Maximum longitude of grid used to calculate ground magnetic perturbations.

Latitude spacing in grid used to calculate ground magnetic perturbations.

Longitude spacing in grid used to calculate ground magnetic perturbations.

Time interval between calculation and output of ground magnetic perturbations.

Comma-separated list of satellite names

Flag indicating whether to generate output files along the trajectory of the tracked satellites

Number of steps between outputs when calculating magnetic perturbations on grid of locations

Flag indicating whether to provide CDF output files

Flag indicating whether to generate HDF output files

Flag indicating whether to generate magnetometer output files

Flag indicating whether to run field line tracer to calculate polar cap (region with open field lines).

Flag indicating whether this is an exoplanetary run

Inner magnetosphere model name

Inner magnetosphere model version

Inner boundary radius

Inner boundary current radius

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.

Density at the inner boundary (1.25 Re)

Temperature at the inner boundary (1.25 Re)

Radiation belt model name

Radiation belt model version

Type of the run - either driven by real data or by artificial conditions

The name of the preset used for the run

Flag indicating whether to run Ring Current Model