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Context. While the shapes of many observed bow shocks can be reproduced bysimple astrosphere models, more elaborate approaches have recently been used toexplain differing observable structures. Aims. By placing perturbations of anotherwise homogeneous interstellar medium in front of the astrospheric bowshock of the runaway blue supergiant $\lambda$ Cephei, the observable structureof the model astrosphere is significantly altered, providing insight into theorigin of perturbed bow shock images. Methods. Three-dimensional single-fluidmagnetohydrodynamic (MHD) models of stationary astrospheres were subjected tovarious types of perturbations and simulated until stationarity was reachedagain. As examples, simple perturbations of the available MHD parameters(number density, bulk velocity, temperature, and magnetic field) as well as amore complex perturbation were chosen. Synthetic observations were generated byline-of-sight integration of the model data, producing H$\alpha$, $70\,\mu$mdust emission, and bremsstrahlung maps of the perturbed astrosphere'sevolution. Results. The resulting shock structures and observational imagesdiffer strongly depending on the type of the injected perturbation and theviewing angles, forming arc-like protrusions or bifurcations of the bow shockstructure, as well as rings, arcs, and irregular structures detached from thebow shock.

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