Simulating observable structures due to a perturbed interstellar medium in front of astrospheric bow shocks in 3D MHD

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Table 2

Boundary values chosen for the model of λ Cephei.

Variable		SW	ISM
r	[pc]	0.05	5
n	[cm⁻³]	3.4	11
u	[km s⁻¹]	2500	80
T	[10³ K]	10	9
B	[nT]	3 × 10⁻³	1
ϑ_u	[°]		90
φ_u	[°]		180
ϑ_B	[°]		30
φ_B	[°]		150

Notes. n, T, u, and B are the number density, temperature, bulk speed, and magnetic flux density, respectively. r is the radius at which the respective boundary conditions are met. ϑ_u,B and φ_u,B are the angles of the homogeneous ISM.

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