Galactica > Solar Physics > Cosmic Rays > D10: Dipole of strong magnetic amplitude

Summary

This simulation corresponds to a dipolar configuration with a high magnetic amplitude (5 Gauss at the poles).

It is a snapshot of the relaxed state after 500 PLUTO times (~10 days).

It is performed in 2.5D (3D vectors computed on a 2D grid).

The grid dimension is 256x256 in spherical coordinates (radius and co-latitude).

The cosmic rays energies probed for this specific configuration are: [$1.0 \, 10^6, 1.0 \, 10^7, 1.0 \, 10^8, 4.45 \, 10^8, 1.0 \, 10^9, 1.0 \, 10^{10}, 1.0 \, 10^{11}$] MV.

Simulated using PLUTO 4.2

Parameters

Parameter	Value
T_corona	$1600000$
Gamma	$1.05$
Rot_rate	$2.6e-06$
N_corona	$100000000$

Algorithms

Structured grid method: Stretched grid in radius, uniform grid in co-latitude and longitude.
Harten-Lax-van Leer-Contact Riemann solver: HLL algorithm for shocks.
Runge-Kutta method: Runge-Kutta of order 2 for time evolution.

Applied physics

Magnetohydrodynamics: MagnetoHydroDynamics

Results

Physical Quantities

Physical quantities of the inner heliosphere from the solar corona to the Earth orbit.

Datafiles:

Vr

Radial velocity of the solar wind (cm/s)

PNG

Vt

Latitudinal velocity of the solar wind (cm/s)

PNG

Vp

Longitudinal velocity of the solar wind (cm/s)

PNG

Br

Radial magnetic field of the star (G)

PNG

Bt

Latitudinal magnetic field of the star (G)

PNG

Bp

Longitudinal magnetic field of the star (G)

PNG

Rho

Density of the solar wind (g/cm^3)

PNG

Prs

Pressure of the solar wind (dyne/cm^2)

PNG

Zoomed physical Quantities

Zoomed physical quantities of the inner heliosphere from to focus on the solar corona structures.

Datafiles:

Vr_zoom

Zoomed radial velocity of the solar wind (cm/s)

PNG

Vt_zoom

Zoomed latitudinal velocity of the solar wind (cm/s)

PNG

Vp_zoom

Zoomed longitudinal velocity of the solar wind (cm/s)

PNG

Br_zoom

Zoomed radial magnetic field of the star (G)

PNG

Bt_zoom

Zoomed latitudinal magnetic field of the star (G)

PNG

Bp_zoom

Zoomed longitudinal magnetic field of the star (G)

PNG

Rho_zoom

Zoomed density of the solar wind (g/cm^3)

PNG

Prs_zoom

Zoomed pressure of the solar wind (dyne/cm^2)

PNG

Parallel Mean Free Path (mfp)

Parallel mean free path of cosmic rays (protons) with various energies propagating in the inner heliosphere from the solar corona to the Earth orbit.

Datafiles:

Lambda_par_1MV

Parallel mfp for a particle with rigidity of 1 MV (AU)

PNG

Lambda_par_zoom_1MV

Zoom on parallel mfp for a particle with rigidity of 1 MV (AU)

PNG

Lambda_par_10MV

Parallel mfp for a particle with rigidity of 10 MV (AU)

PNG

Lambda_par_zoom_10MV

Zoom on parallel mfp for a particle with rigidity of 10 MV (AU)

PNG

Lambda_par_100MV

Parallel mfp for a particle with rigidity of 100 MV (AU)

PNG

Lambda_par_zoom_100MV

Zoom on parallel mfp for a particle with rigidity of 100 MV (AU)

PNG

Lambda_par_400MV

Parallel mfp for a particle with rigidity of 400 MV (AU)

PNG

Lambda_par_zoom_400MV

Zoom on parallel mfp for a particle with rigidity of 400 MV (AU)

PNG

Lambda_par_1e3MV

Parallel mfp for a particle with rigidity of 1e3 MV (AU)

PNG

Lambda_par_zoom_1e3MV

Zoom on parallel mfp for a particle with rigidity of 1e3 MV (AU)

PNG

Lambda_par_1e4MV

Parallel mfp for a particle with rigidity of 1e4 MV (AU)

PNG

Lambda_par_zoom_1e4MV

Zoom on parallel mfp for a particle with rigidity of 1e4 MV (AU)

PNG

Lambda_par_1e5MV

Parallel mfp for a particle with rigidity of 1e5 MV (AU)

PNG

Lambda_par_zoom_1e5MV

Zoom on parallel mfp for a particle with rigidity of 1e5 MV (AU)

PNG

Perpendicular Mean Free Path (mfp)

Perpendicular mean free path of cosmic rays (protons) with various energies propagating in the inner heliosphere from the solar corona to the Earth orbit.