Table 1
Main parameters of the simulations discussed in the paper.
Run | rmax | (Nr, Nθ, Nϕ) | n0 | p0 | BI | B0 | Ω |
---|---|---|---|---|---|---|---|
1 no wind | 26 | (24 geom,24,48) | 4 | 0.24 | 0 | 100 | 0.78 |
2 – wind | 54 | (20 geom,16,32) | 1 | 0.59 | 0 | 1648 | 3.14 |
3 – wind + IMF Y | 54 | (20 geom,16,32) | 1 | 0.59 | 3.46 | 1648 | 3.14 |
4 – wind | 54 | (96 const,24,48) | 1 | 1 | 0 | 1648 | 6.42 |
Notes.The plasma surrounding the rotating dipole is characterised by a magnetic field intensity
BI, a number density
nI = 1, a sound speed
cs,I = 1, and a fluid velocity
vI = 20 (except for simulation 1 where
vI = 0). Normalisation is such that
is the Alfvén velocity and
, the sound speed (here we use γ = 5∕3). The numerical grid is a spherical regular one with Nr, Nθ, Nϕ grid points. Grid points spacing is constant in θ and ϕ, and it is either constant (“const”) or geometrically increasing away from the centre (“geom”). Quantities n0, p0 refer to the plasma density and pressure at the inner boundary (the planetary surface, located at r = 1). B0 is the dipole strength at the magnetic equator and distance r = 1. Finally, Ω is the angular velocity of the rotating dipole.
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