A hydrodynamical model of the circumstellar bubble created by two massive stars

Abstract

Numerical models of the wind-blown bubble of massive stars usually only account for the wind of a single star. However, since massive stars are usually formed in clusters, it would be more realistic to follow the evolution of a bubble created by several stars. We develope a two-dimensional (2D) model of the circumstellar bubble created by two massive stars, a 40 solar mass star and a 25 solar mass star, and follow its evolution. The stars are separated by approximately 16 pc and surrounded by a cold medium with a density of 20 particles per cubic cm. We use the MPI-AMRVAC hydrodynamics code to solve the conservation equations of hydrodynamics on a 2D cylindrical grid using time-dependent models for the wind parameters of the two stars. At the end of the stellar evolution (4.5 and 7.0 million years for the 40 and 25 solar mass stars, respectively), we simulate the supernova explosion of each star. Each star initially creates its own bubble. However, as the bubbles expand they merge, creating a combined, aspherical bubble. The combined bubble evolves over time, influenced by the stellar winds and supernova explosions. The evolution of a wind-blown bubble created by two stars deviates from that of the bubbles around single stars. In particular, once one of the stars has exploded, the bubble is too large for the wind of the remaining star to maintain and the outer shell starts to disintegrate. The lack of thermal pressure inside the bubble also changes the behavior of circumstellar features close to the remaining star. The supernovae are contained inside the bubble, which reflects part of the energy back into the circumstellar medium.

Accepted for publication in A&A. Six .avi files to be published online (uploaded to ArXiv DC and available as ancillary files) (updated after language corrections)

References in corpus (5)

• The Evolution of Supernovae in Circumstellar Wind Bubbles II: Case of a Wolf-Rayet star
• Numerical models of collisions between core-collapse supernovae and circumstellar shells
• Radiation-Hydrodynamic Models of the evolving Circumstellar Medium around Massive Stars
• Thin shell morphology in the circumstellar medium of massive binaries
• Discovery of Twin Wolf-Rayet Stars Powering Double Ring Nebulae

Cited by in corpus (14)

• Superbubble dynamics in globular cluster infancy II. Consequences for secondary star formation in the context of self-enrichment via fast rotating massive stars
• Nonthermal particles and photons in starburst regions and superbubbles
• Coupling hydrodynamics with comoving frame radiative transfer: I. A unified approach for OB and WR stars
• Cosmic Ray Models
• Shape and evolution of wind-blown bubbles of massive stars: on the effect of the interstellar magnetic field
• Multi-dimensional models of circumstellar shells around evolved massive stars
• Dynamics and Energy Loss in Superbubbles
• 3D MHD astrospheres: applications to IRC-10414 and Betelgeuse
• Circum-stellar medium around rotating massive stars at solar metallicity
• High-energy neutrinos from Galactic superbubbles
• Self-Sealing Shells: Blowouts and Blisters on the Surfaces of Leaky Wind-Blown-Bubbles and Supernova Remnants
• The Exceptional X-ray Evolution of SN1996cr in High Resolution
• How does the stellar wind influence the radio morphology of a supernova remnant?
• Discovery of an optical cocoon tail behind the runaway HD 185806