Impact of solar-wind turbulence on a planetary bow shock - A global 3D simulation

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Volume 692 (December 2024)

A&A, 692 (2024) A53

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Table 1

Input parameters of the simulations.

Variable	Unit	Value	Description
Normalisation
Density	n₀		Initial solar-wind density
Magnetic field	B₀		Magnitude of the average solar-wind magnetic field
Time	$Ω_{c i}^{- 1}$ ${\rm{\Omega }}_{ci}^{ - 1}$	m_pc / eB₀	Inverse of proton gyrofrequency
Speed	C_A	$B_{0} / \sqrt{4 π n_{0} m_{p}}$ ${B_0}/\sqrt {4\pi {n_0}{m_p}}$	Alfvén speed
Length	d_i	C_A/Ω_ci	Proton inertial length
Pressure	P₀	$n_{0} m_{p} C_{A}^{2}$ ${n_0}{m_p}C_A^2$	Normalizing pressure

Solar-wind parameters
n_sw	n₀	1.0	Solar-wind proton density
B_sw	B₀	$(\frac{1}{\sqrt{2}}, \frac{1}{\sqrt{2}}, 0)$ $\left( {{1 \over {\sqrt 2 }},{1 \over {\sqrt 2 }},0} \right)$	Solar-wind magnetic field vector
U_sw	C_A	(–10, 0, 0)	Solar-wind velocity vector in the planet’s reference frame
T_i/T_e	_–	1.0	Ratio of proton temperature to electron temperature
β = βi + β_e	_–	1.0	Solar wind plasma beta
Y_e	–	d align="right">1.0	Electron adiabatic index
C_s	C_A	1.4	Solar-wind sound speed
C_ms	C_A	1.7	Solar-wind magnetosonic speed
M_A	–	10	Bow shock Mach number

Turbulence
δB₀/ B₀	_–	0.54	Initial magnetic field fluctuations
δv₀/C_A	–	0.54	Initial velocity fluctuations

Magnetized planet
(X_P, Y_P, Z_p)	d_i	$(\frac{3 L_{b o x}}{8}, \frac{L_{b o x}}{2}, \frac{L_{b o x}}{2})$ $\left( {{{3{L_{box}}} \over 8},{{{L_{box}}} \over 2},{{{L_{box}}} \over 2}} \right)$	Position of the planet’s centre in simulation box
τ_dip	_–	(0, –1, 0)	Dipole moment direction
D_p	d_i	200	Distance to the magnetopause from the planet’s centre

Grid and numerics
∆X = ∆Y = ∆Z	d_i	5.0	Grid resolution
∆t	$Ω_{c i}^{- 1}$ ${\rm{\Omega }}_{ci}^{ - 1}$	0.5	Time resolution
L_box = L_X = L_Y = L_Z	d_i	2000	Box size in each spatial direction
N_pcc	_–	600	Number of particles per cell
η_hup	–	0.01	Numerical hyper-resistivity

Simulation names
Sim 1			Decaying solar-wind turbulence
Sim 2.1			Turbulent solar wind vs. planet
Sim 2.2			Laminar solar wind vs. planet

Notes. Code normalizations, solar-wind parameters for all runs, initial amplitude of turbulence in the decaying run, characteristics of the magnetized planet, grid and time resolution for all runs. m_p is the proton mass, c the speed of light in vacuum, and e the elementary charge. Simulation parameters are typical of the solar wind (Owens et al. 2023), with n0 and B0 being the initial solar-wind density and the magnetic field magnitude.

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