Research Overview:

The submitted is the data used to plot figures 7 and 8 of the paper "Application of the Monte Carlo method in modeling dusty gas, dust in plasma, and energetic ions in planetary, magnetospheric, and heliospheric  environments."  The paper's main focus is documenting Monte Carlo code Adaptive Mesh Particle Simulator (AMPS) developed at the University of Michigan. The goal of documenting the code is to make it usable by the community. The presented figures are illustrations of the prior application of the code. In particular, the submitted are the results from research related to investigating 1) the structure of hot oxygen corona of Mars, 2) propagation of the energetic particles of solar and galactic origin in the Earth's magnetosphere, and 3) calculation of the variability of the cutoff rigidity of energetic parties at the top of the Earth's atmosphere.

Methods:
In this research, we have used the Monte Carlo code Adaptive Mesh Particle Simulator (AMPS).  The essence of the approach is that the dusty gas or plasma are represented by many model particles affected by the same physics laws as real ions, dust particles, or gas molecules. Such an approach allows one to included kinetic effects in a numerical model that go beyond physics described with fluid methods. 

Adaptive Mesh Particle Simulator (AMPS) was developed as a general-purpose code for solving the Boltzmann equation in conditions typical for planetary and planetary satellite exospheres. Later, the code was generalized to model dusty gas, dust, and plasma and simulate solar energetic particles' transportation and galactic cosmic rays in planetary magnetospheres.  The code is documented in Tenishev et al., "Kinetic modeling of sodium in the lunar exosphere", Icarus, Volume 226, Issue 2, November–December 2013, Pages 1538-1549 and Tenishev et al., "Application of the Monte Carlo method in modeling dusty gas, dust in plasma, and energetic ions in planetary, magnetospheric, and heliospheric environments" submitted to JGR-Space, 2020.

File Inventory

The submitted data illustrates some of the prior applications of AMPS. Here is the file inventory: 
fig7a.tar contains the energy distribution function of galactic cosmic ray protons at various locations in the Earth's magnetosphere for a set of the simulation times.
fig7b.tar is a file containing trajectories of the energetic protons as they move toward the Earth.
fig8.tar contains maps of the cutoff rigidity at the altitude of 500 km before and after the magnetospheric storm on March 17, 2015.


Definition of Terms and Variables

X, Y, Z - location in the Earth's magnetosphere
E - energy
f(E) - the value of the energy distribution function
Fluency(E) - the fluency of the energetic protons with a particular energy
Cutoff Rigidity - the cutoff rigidity at a particular location in the Earth's magnetosphere 
Injected Particle Number - the number of the model particles used for calculating the cutoff rigidity at a specific location in the Earth's magnetosphere.
v[m/s] - particle velocity
Max energy injected particles - the maximum eagerly of a model particle injected into the simulation when calculating the cutoff rigidity at a particular plan in the Earth's magnetosphere 

Use and Access
All submitted files can be visualized with Tecplot or Visit visualization packages.