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The winds of massive stars create large (>10 pc) bubbles around theirprogenitors. As these bubbles expand they encounter the interstellar coherentmagnetic field which, depending on its strength, can influence the shape of thebubble. We wish to investigate if, and how much, the interstellar magneticfield can contribute to the shape of an expanding circumstellar bubble around amassive star. We use the MPI-AMRVAC code to make magneto-hydrodynamicalsimulations of bubbles, using a single star model, combined with severaldifferent field strengths: B = 5, 10, and 20 muG for the interstellar magneticfield. This covers the typical field strengths of the interstellar magneticfields found in the galactic disk and bulge. Furthermore, we present twosimulations that include both a 5 muG interstellar magnetic field and a 10,000K interstellar medium and two different ISM densities to demonstrate how themagnetic field can combine with other external factors to influence themorphology of the circumstellar bubbles. Our results show that low magneticfields, as found in the galactic disk, inhibit the growth of the circumstellarbubbles in the direction perpendicular to the field. As a result, the bubblesbecome ovoid, rather than spherical. Strong interstellar fields, such asobserved for the galactic bulge, can completely stop the expansion of thebubble in the direction perpendicular to the field, leading to the formation ofa tube-like bubble. When combined with a warm, high-density ISM the bubble isgreatly reduced in size, causing a dramatic change in the evolution oftemporary features inside the bubble. The magnetic field of the interstellarmedium can affect the shape of circumstellar bubbles. This effect may haveconsequences for the shape and evolution of circumstellar nebulae and supernovaremnants, which are formed within the main wind-blown bubble.

Shape and evolution of wind-blown bubbles of massive stars: on the effect of the interstellar magnetic field