Radiation-Hydrodynamic Simulations of Interstellar and Circumstellar Bubbles

Po-Sheng Ou^1*, Ke-Jung Chen¹

¹Institute of Astronomy and Astrophysics, Academia Sinica, Taipei, Taiwan

* Presenter:Po-Sheng Ou, email:psou@asiaa.sinica.edu.tw

Massive stars can lose large fractions of mass through stellar winds. These materials form circumstellar medium (CSM) and generate interstellar and circumstellar bubbles. In this work, we systematically study stellar mass loss and formation of bubbles from the main sequence to the Wolf-Rayet (WR) phase. First we use the MESA code to produce a grid of ~2000 stellar models with various initial masses and metallicities. From these models, we calculate the total mass loss and energy feedback during the stellar lifetimes. The mass-loss rates and wind velocities as functions of time are obtained from the stellar models, and then imported into the radiation hydrodynamic simulations with the RAMSES code. Using these realistic mass-loss rates, we build up models of wind-blown bubbles. We analyze the structures of interstellar and circumstellar bubbles around WR stars and compare them with the bubbles observed in the Milky Way Galaxy and the Large Magellanic Cloud.

Keywords: Interstellar bubbles, Circumstellar medium, Stellar wind, Wolf-Rayet stars