author={Jonathan Mackey and Shazrene Mohamed and Hilding R. Neilson and Norbert Langer and Dominique M.-A. Meyer},
  journal={The Astrophysical Journal Letters},
A significant fraction of massive stars are moving supersonically through the interstellar medium (ISM), either due to disruption of a binary system or ejection from their parent star cluster. The interaction of their wind with the ISM produces a bow shock. In late evolutionary stages these stars may undergo rapid transitions from red to blue and vice versa on the Hertzsprung–Russell diagram, with accompanying rapid changes to their stellar winds and bow shocks. Recent three-dimensional… 

Numerical models for the circumstellar medium around Betelgeuse

The nearby red supergiant (RSG) Betelgeuse has a complex circumstellar medium out to at least 0.5 parsecs from its surface, shaped by its mass-loss history within the past  ≈ 0.1 Myr, its

Interacting supernovae from photoionization-confined shells around red supergiant stars

A model in which Betelgeuse’s wind is photoionized by radiation from external sources can explain the static shell without requiring a new understanding of the bow shock, providing a natural explanation for the many supernovae that have signatures of circumstellar interaction.

Models of the circumstellar medium of evolving, massive runaway stars moving through the Galactic plane

At least 5 per cent of the massive stars are moving supersonically through the interstellar medium (ISM) and are expected to produce a stellar wind bow shock. We explore how the mass-loss and space

The Circumstellar Medium of Massive Stars in Motion

The circumstellar medium around massive stars is strongly impacted by stellar winds, radiation, and explosions. We use numerical simulations of these interactions to constrain the current properties

Using numerical models of bow shocks to investigate the circumstellar medium of massive stars

Many massive stars travel through the interstellar medium at supersonic speeds. As a result they form bow shocks at the interface between the stellar wind. We use numerical hydrodynamics to reproduce

Modeling nonthermal emission from stellar bow shocks

Runaway O- and early B-type stars passing throughout the interstellar medium at supersonic velocities and characterized by strong stellar winds may produce bow shocks that can serve as particle

Bow shock nebulae of hot massive stars in a magnetized medium

A significant fraction of OB-type, main-sequence massive stars are classified as runaway and move supersonically through the interstellar medium (ISM). Their strong stellar winds interact with their

IRC 10414: a bow-shock-producing red supergiant star ⋆

Most runaway OB stars, like the majority of massive stars residing in their parent clusters, go through the red supergiant (RSG) phase during their lifetimes. Nonetheless, although many dozens of

Asymmetric supernova remnants generated by Galactic, massive runaway stars

After the death of a runaway massive star, its supernova shock wave interacts with the bow shocks produced by its defunct progenitor, and may lose energy, momentum, and its spherical symmetry before

Can the magnetic field in the Orion arm inhibit the growth of instabilities in the bow shock of Betelgeuse

Many evolved stars travel through space at supersonic velocities, which leads to the formation of bow shocks ahead of the star where the stellar wind collides with the interstellar medium (ISM).



3D simulations of Betelgeuse’s bow shock

Betelgeuse, the bright, cool red supergiant in Orion, is moving supersonically relative to the local interstellar medium. The star emits a powerful stellar wind that collides with this medium,

Search for OB stars running away from young star clusters - I. NGC 6611

N-body simulations have shown that the dynamical decay of the young (∼1 Myr) Orion Nebula cluster could be responsible for the loss of at least half of its initial content of OB stars. This result

Interstellar Weather Vanes: GLIMPSE Mid-Infrared Stellar Wind Bow Shocks in M17 and RCW 49

We report the discovery of six infrared stellar wind bow shocks in the Galactic massive star formation regions M17 and RCW 49 from Spitzer GLIMPSE (Galactic Legacy Infrared Mid-Plane Survey

Massive Stars and the Energy Balance of the Interstellar Medium. I. The Impact of an Isolated 60 M☉ Star

We present results of numerical simulations carried out with a two-dimensional radiation hydrodynamics code in order to study the impact of massive stars on their surrounding interstellar medium.

The circumstellar environment of Wolf–Rayet stars and gamma‐ray burst afterglows

We study the evolution of the circumstellar medium of massive stars. We pay particular attention to Wolf-Rayet stars that are thought to be the progenitors of some long Gamma-Ray Bursts. We detail

An IRAS/ISSA Survey of Bow Shocks Around Runaway Stars

We searched for bow shock-like objects like those known around Oph and a Cam near the positions of 183 runaway stars. Based primarily on the presence and morphology of excess 60 micron emission we

Runaway stars as progenitors of supernovae and gamma-ray bursts

When a core-collapse supernova occurs in a binary system, the surviving star as well as the compact remnant emerging from the supernova may reach a substantial space velocity. With binary population

Forming a constant density medium close to long gamma-ray bursts

Aims. The progenitor stars of long Gamma-Ray Bursts (GRBs) are thought to be Wolf-Rayet stars, which generate a massive and energetic wind. Nevertheless, about 25 percent of all GRB afterglows light

Exact Analytic Solutions for Stellar Wind Bow Shocks

Stellar wind bow shocks have been seen in association with a wide variety of stellar objects, from pulsars to young stars. A new solution method is presented for bow shocks in the thin-shell limit,


We study the hydrodynamical behavior of the gas expelled by moving asymptotic giant branch stars interacting with the interstellar medium (ISM). Our models follow the wind modulations prescribed by