This dataset contains the program codes, numerical data, and figures created and used in the paper ``Nonlinear Dynamics and Auroral Acceleration Processes of Electrons Driven by Kinetic Alfvén Waves in the Magnetosphere'' by K. Saito et al. (2025).The zip file open_source_in_zenodo.tar.bz2 contains the following directories and files.program_code: Python programs to create the figures from the numerical data files in other directories. test_particle_simulation_Section3_forpaper/(initial wave phase per pi)pi/(initial kinetic energy)eV(initial pitch angle)deg_1.00deg(.nc/.png/contour.png): Numerical data files (netCDF4), PNG figures about electron trajectories, and the force of a parallel electric field component, such as in Figures 3-5.These figures are created by the program of program_code/test_particle_simulation_Section3_plot_for_paper.py. test_particle_simulation_detrapped_phase_edgedefinition_forpaper/auroral_precipitation/: Numerical data file and PNG figures in Figures 8 and 9.Figure 8 is created by the program of program_code/initial_position_of_precipitating_electrons_plot_for_paper.py.Figure 9 is created by the program of program_code/test_particle_simulation_detrapped_phase_edgedefinition_auroral_precipitation_for_paper.py. test_particle_simulation_detrapped_phase_edgedefinition_forpaper/Kperp_eq_1.0000_1000.0000_eV_S_0.1000_1.0000_20_10_linear_psi_exit(-1.00/-10.00)forpaper/Kperp_eq(electron perpendicular kinetic energy at the equator)eV_S_(initial S value)psi_exit(-1.00/-10.00).(nc/png): Numerical data files and PNG figures in Figure A1 (-1.00) and Figure 10 (-10.00).These figures are created by the program of program_code/test_particle_simulation_detrapped_phase_edgedefinition_plot_for_paper.py.

This dataset contains the program codes, numerical data, and figures created and used in the paper ``Nonlinear Dynamics and Auroral Acceleration Processes of Electrons Driven by Kinetic Alfvén Waves in the Magnetosphere'' by K. Saito et al. (2025).The zip file open_source_in_zenodo.tar.bz2 contains the following directories and files.program_code: Python programs to create the figures from the numerical data files in other directories. test_particle_simulation_Section3_forpaper/(initial wave phase per pi)pi/(initial kinetic energy)eV(initial pitch angle)deg_1.00deg(.nc/.png/contour.png): Numerical data files (netCDF4), PNG figures about electron trajectories, and the force of a parallel electric field component, such as in Figures 3-5.These figures are created by the program of program_code/test_particle_simulation_Section3_plot_for_paper.py. test_particle_simulation_detrapped_phase_edgedefinition_forpaper/auroral_precipitation/: Numerical data file and PNG figures in Figures 8 and 9.Figure 8 is created by the program of program_code/initial_position_of_precipitating_electrons_plot_for_paper.py.Figure 9 is created by the program of program_code/test_particle_simulation_detrapped_phase_edgedefinition_auroral_precipitation_for_paper.py. test_particle_simulation_detrapped_phase_edgedefinition_forpaper/Kperp_eq_1.0000_1000.0000_eV_S_0.1000_1.0000_20_10_linear_psi_exit(-1.00/-10.00)forpaper/Kperp_eq(electron perpendicular kinetic energy at the equator)eV_S_(initial S value)psi_exit(-1.00/-10.00).(nc/png): Numerical data files and PNG figures in Figure A1 (-1.00) and Figure 10 (-10.00).These figures are created by the program of program_code/test_particle_simulation_detrapped_phase_edgedefinition_plot_for_paper.py.

This dataset contains the plasma distribution data in the Jupiter–Io system, calculated from the Plasma Distribution Solver and used for figures in the paper “Plasma Distribution Solver: A model for field-aligned plasma profiles based on spatial variation of velocity distribution functions” by K. Saito et al. (2023). The contents of files ‘all_Case_1.csv’ and ‘all_Case_2.csv’ are as follows: Position along the magnetic field line (0 at the magnetic equator) [m] (column 1) Distance from the Jovian center [km] (column 2) Magnetic latitude rad (column 3(4)) Magnetic flux density [T] (column 5) The initial condition of electrostatic potential [V] (column 6) The result of electrostatic potential [V] (column 7) Number density profiles [m^-3] (columns 8-17) Charge density profiles obtained from the integration of velocity distribution functions [C m^-3] (column 18) Charge density profiles obtained from Poisson’s equation [C m^-3] (column 19) Convergence value (column 20) Particle flux density [m^-2 s^-1] (columns 21-30) Mean flow velocity parallel to the field line [m s^-1] (columns 31-40) Plasma pressure perpendicular to the field line [Pa] (columns 41-50) Plasma pressure parallel to the field line [Pa] (columns 51-60) Plasma dynamic pressure [Pa] (columns 61-70) Perpendicular temperature [J] (columns 71-80) Parallel temperature [J] (columns 81-90) Alfvén speed considering the displacement current term in Ampère’s law [m s^-1] (column 91) Alfvén speed per the speed of light (column 92) Ion inertial length using averaged mass [m] (column 93) Electron inertial length [m] (column 94) Ion Larmor radius using averaged mass [m] (column 95) Ion acoustic gyroradius using averaged mass [m] (column 96) Electron Larmor radius [m] (column 97) Current density [A m^-2] (column 98) The Python codes ‘plot_all.py,’ ‘plot_plasma_beta_comparison.py,’ and ‘plot_Alfven_speed_comparison.py’ can plot Figures 5, 6, 7, and 9 of the paper using the above CSV files. The files ‘boundary_conditions_Case_1.csv’ and ‘boundary_conditions_Case_2.csv’ contain the boundary conditions for Cases 1 and 2. The zip files ‘probability_density_function_Case_1_H_Io.zip’ and ‘probability_density_function_Case_1_H_Jupiter_North.zip’ are zipped CSV files with the same name. The contents of these files are as follows: Magnetic latitude [degree] (column 1) Perpendicular velocity at the particle position [m s^-1] (column 2) Parallel velocity at the particle position [m s^-1] (column 3) Perpendicular velocity at the boundary [m s^-1] (column 4) Parallel velocity at the boundary [m s^-1] (column 5) Probability density function [s³ m^-3] (column 6) Differential flux per number density [cm^-2 s^-1 sr^-1 keV^-1] (column 7) The Python code ‘plot_velocity_distribution_function.py’ can plot Figure 8 of the paper using this CSV file.

This dataset contains the plasma distribution data in the Jupiter–Io system, calculated from the Plasma Distribution Solver and used for figures in the paper “Plasma Distribution Solver: A model for field-aligned plasma profiles based on spatial variation of velocity distribution functions” by K. Saito et al. (2023). The contents of files ‘all_Case_1.csv’ and ‘all_Case_2.csv’ are as follows: Position along the magnetic field line (0 at the magnetic equator) [m] (column 1) Distance from the Jovian center [km] (column 2) Magnetic latitude rad (column 3(4)) Magnetic flux density [T] (column 5) The initial condition of electrostatic potential [V] (column 6) The result of electrostatic potential [V] (column 7) Number density profiles [m^-3] (columns 8-17) Charge density profiles obtained from the integration of velocity distribution functions [C m^-3] (column 18) Charge density profiles obtained from Poisson’s equation [C m^-3] (column 19) Convergence value (column 20) Particle flux density [m^-2 s^-1] (columns 21-30) Mean flow velocity parallel to the field line [m s^-1] (columns 31-40) Plasma pressure perpendicular to the field line [Pa] (columns 41-50) Plasma pressure parallel to the field line [Pa] (columns 51-60) Plasma dynamic pressure [Pa] (columns 61-70) Perpendicular temperature [J] (columns 71-80) Parallel temperature [J] (columns 81-90) Alfvén speed considering the displacement current term in Ampère’s law [m s^-1] (column 91) Alfvén speed per the speed of light (column 92) Ion inertial length using averaged mass [m] (column 93) Electron inertial length [m] (column 94) Ion Larmor radius using averaged mass [m] (column 95) Ion acoustic gyroradius using averaged mass [m] (column 96) Electron Larmor radius [m] (column 97) Current density [A m^-2] (column 98) The Python codes ‘plot_all.py,’ ‘plot_plasma_beta_comparison.py,’ and ‘plot_Alfven_speed_comparison.py’ can plot Figures 5, 6, 7, and 9 of the paper using the above CSV files. The files ‘boundary_conditions_Case_1.csv’ and ‘boundary_conditions_Case_2.csv’ contain the boundary conditions for Cases 1 and 2. The zip files ‘probability_density_function_Case_1_H_Io.zip’ and ‘probability_density_function_Case_1_H_Jupiter_North.zip’ are zipped CSV files with the same name. The contents of these files are as follows: Magnetic latitude [degree] (column 1) Perpendicular velocity at the particle position [m s^-1] (column 2) Parallel velocity at the particle position [m s^-1] (column 3) Perpendicular velocity at the boundary [m s^-1] (column 4) Parallel velocity at the boundary [m s^-1] (column 5) Probability density function [s³ m^-3] (column 6) Differential flux per number density [cm^-2 s^-1 sr^-1 keV^-1] (column 7) The Python code ‘plot_velocity_distribution_function.py’ can plot Figure 8 of the paper using this CSV file.