Volume 584, December 2015
|Number of page(s)||21|
|Section||Interstellar and circumstellar matter|
|Published online||18 November 2015|
Shape and evolution of wind-blown bubbles of massive stars: on the effect of the interstellar magnetic field⋆
1 KU Leuven, Centre for mathematical Plasma Astrophysics, Celestijnenlaan 200B, 3001 Leuven, Belgium
2 KU Leuven, Institute of Astronomy, Celestijnenlaan 200D, 3001 Leuven, Belgium
3 LuTh, Observatoire de Paris, 5 place Jules Janssen, 92195 Meudon, France
4 LUTh, Observatoire de Paris, CNRS/INSU, PSL, Sorbonne Paris Cité, 75074 Paris, France
5 APC, Université Paris Diderot, 10 rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France
6 Laboratoire Univers et Particules (LUPM) Université Montpellier, CNRS/IN2P3, CC72, place Eugène Bataillon, 34095 Montpellier Cedex 5, France
Received: 28 October 2014
Accepted: 1 September 2015
Context. The winds of massive stars create large (>10 pc) bubbles around their progenitors. As these bubbles expand they encounter the interstellar coherent magnetic field which, depending on its strength, can influence the shape of the bubble.
Aims. We wish to investigate if, and how much, the interstellar magnetic field can contribute to the shape of an expanding circumstellar bubble around a massive star.
Methods. We use the MPI-AMRVAC code to make magneto-hydrodynamical simulations of bubbles, using a single star model, combined with several different field strengths: B = 5, 10, and 20 μG for the interstellar magnetic field. This covers the typical field strengths of the interstellar magnetic fields found in the galactic disk and bulge. Furthermore, we present two simulations that include both a 5 μG interstellar magnetic field and a warm (10 000 K) interstellar medium (ISM) and two different ISM densities to demonstrate how the magnetic field can combine with other external factors to influence the morphology of the circumstellar bubbles.
Results. Our results show that low magnetic fields, as found in the galactic disk, inhibit the growth of the circumstellar bubbles in the direction perpendicular to the field. As a result, the bubbles become ovoid, rather than spherical. Strong interstellar fields, such as observed for the galactic bulge, can completely stop the expansion of the bubble in the direction perpendicular to the field, leading to the formation of a tube-like bubble. When combined with an ISM that is both warm and high density the bubble is greatly reduced in size, causing a dramatic change in the evolution of temporary features inside the bubble such as Wolf-Rayet ring nebulae.
Conclusions. The magnetic field of the interstellar medium can affect the shape of circumstellar bubbles. This effect may have consequences for the shape and evolution of circumstellar nebulae and supernova remnants, which are formed within the main wind-blown bubble.
Key words: magnetohydrodynamics (MHD) / circumstellar matter / stars: massive / ISM: bubbles / ISM: magnetic fields / ISM: structure
Appendices and movies associated to Figs. A.1−A.12 are available in electronic form at http://www.aanda.org
© ESO, 2015
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.