EPREM model run submission page

REQUEST an EPREM MODEL RUN

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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, 0.001 ≤ X ≤ 1
, -10 ≤ X ≤ 10
cm^-3, 1 ≤ X ≤ 20
G, 8.00E-06 ≤ X ≤ 3.20E-05
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 ≤ 360
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).
1/AU, 0 ≤ X ≤ 1
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
, 0.1 ≤ X ≤ 10
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
    AU, 0.0930094 ≤ X ≤ 5
    degrees, -90 ≤ X ≤ 90
    degrees, 0 ≤ X ≤ 360
Heliosphere Setup

These parameters define our heliosphere for the model.

AU, 0.00465047 ≤ X ≤ 0.0930094
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
, 0.001 ≤ X ≤ 1
, 1.5 ≤ X ≤ 2
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
    nucleons, 1 ≤ X ≤ 56
    e, 1 ≤ X ≤ 26
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.