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These parameters provide the basic choices for running the model. These can be used to produce a generally useful output from the model. Advanced parameters are only necessary for fine tuning of the simulation.
Solar Wind and Shock

Parameters for defining the background solar wind (which will be a Parker spiral) and an idealized shock for accelerating particles.

km/s, 200 ≤ X ≤ 800
AU, 0.01 ≤ X ≤ 1
-10 ≤ X ≤ 10
Power-law dependence of mean free path on radial distance
This forces the parallel mean free path to be proportional to an inverse power of the magnetic-field magnitude. The power is equal to -(mean free path radial power)/2.
0 ≤ X ≤ 1
Power-law dependence of mean free path on particle rigidity
n/cm^3, 1 ≤ X ≤ 20
G, 0.000008 ≤ X ≤ 0.000032
This will include an idealized cone shock as an approximation of a CME to accelerate particles from. This is generally recommended to be turned on unless there is a special use case against it.
km/s, 200 ≤ X ≤ 1500
degrees, -90 ≤ X ≤ 90
degrees, 0 ≤ X ≤ 360
degrees, 0 ≤ X ≤ 180
This will define the width of the shock. As the shock is a cone model, it has circular symmetry, so this will be the opening angle in any direction (not only longitude). An opening angle of zero will produce a shock of 360 degrees
degrees, 0 ≤ X ≤ 180
This will define the azimuthal width of the shock. This is used to create an elliptical cone.
degrees, 0 ≤ X ≤ 180
This will define the polar width of the shock. This is used to create an elliptical cone.
1/AU, 0 ≤ X ≤ 1000
This is a scale factor for the shock. Normally the sharpness divided by the scale length.
0.01 ≤ X ≤ 1
Factor defining the sharpness of the shock
AU, 0.0001 ≤ X ≤ 1
Exponential scale length of shock variation
0 ≤ X ≤ 1000
Exponential rate at which shocked quantities return to their upstream values
0.1 ≤ X ≤ 10
Shock density compression ratio
days, 0.1 ≤ X ≤ 3
SEP Energy Spectrum

These parameters define the properties of the output SEP energy spectrum. The minimum and maximum will define the range of the spectrum, while the number of steps will define the number of energy bins in the spectrum.

MeV/nucleon, 0.8 ≤ X ≤ 1000
MeV/nucleon, 25 ≤ X ≤ 3000
2 ≤ X ≤ 30
Point Observers

Defining the position of point observers in the heliosphere. These observers will have measurements of particles and solar wind properties.

0 ≤ X ≤ 10
Heliosphere Setup

These parameters define our heliosphere for the model.

AU, 0.00465 ≤ X ≤ 0.093009
days, 0 ≤ X ≤ 3
days, 1 ≤ X ≤ 20
days, 0.1 ≤ X ≤ 1
days, 0.1 ≤ X ≤ 50
Model Grid

EPREM uses a lagrangian grid, so the nodes are moving with the solar wind. This is different from an Eulerian grid, in which the positions in the heliosphere are fixed. The nodes are on streams that originate as if on faces of a cube. So, for example, 3 rows and 3 columns will produce cube faces with 9 streams, and thus 54 total streams.

1 ≤ X ≤ 9
A greater stream density will make the output more cumbersome to view and process, but will fill in the physical space to a greater degree.
1 ≤ X ≤ 9
A greater stream density will make the output more cumbersome to view and process, but will fill in the physical space to a greater degree.
15 ≤ X ≤ 500
More nodes will make calculation points closer together within a stream, but increase the time to process the data.
Particle Distribution Properties

Parameters for defining various properties of the source particle and SEP particle distributions.

2 ≤ X ≤ 25
n / (cm^2*s*sr*MeV/nuc), 0.01 ≤ X ≤ 10
1.5 ≤ X ≤ 2
For defining the particle source population (before SEP acceleration).
MeV/nucleon, 0 ≤ X ≤ 5
For defining the particle source population (before SEP acceleration).
1.5 ≤ X ≤ 2
For defining the particle source population (before SEP acceleration).
MeV/nucleon, 1 ≤ X ≤ 50
For defining the particle source population (before SEP acceleration).
1 ≤ X ≤ 10
Particle Transport Settings
Controls the ratio of perpendicular to parallel diffusion. Setting to "no" turns it off completely (value=0). If enabled, value must be in the specified range.
0.001 ≤ X ≤ 1
This strength is defined as a fraction of the parallel diffusion strength.
OPTIONAL: SPECIAL REQUEST

ONLY if you require a customized simulation setup not provided by the standard submission options. Unlike the standard runs that are automatically processed, special requests are reviewed and manually modified by the CCMC staff. Please note that special requests are reviewed and manually modified by the CCMC staff and are executed only if resources are available.