• DOI:10.3847/2041-8213/ab7d37
• Corpus ID: 211011050

The Birth of a Massive First-star Binary

@article{Sugimura2020TheBO,
  title={The Birth of a Massive First-star Binary},
  author={Kazuyuki Sugimura and Tomoaki Matsumoto and Takashi Hosokawa and Shingo Hirano and Kazuyuki Omukai},
  journal={arXiv: Astrophysics of Galaxies},
  year={2020}
}

• K. Sugimura, Tomoaki Matsumoto, +2 authors K. Omukai
• Published 31 January 2020
• Physics
• arXiv: Astrophysics of Galaxies

We study the formation of massive Pop III binary stars using a newly developed radiation hydrodynamics code with the adaptive mesh refinement and adaptive ray-tracing methods. We follow the evolution of a typical primordial star-forming cloud obtained from a cosmological hydrodynamics simulation. Several protostars form as a result of disk fragmentation and grow in mass by the gas accretion, which is finally quenched by the radiation feedback from the protostars. Our code enables us, for the first time, to consider the feedback by both the ionizing and dissociating radiation from the multiple protostars, which is essential for self-consistently determining their final masses. At the final step of the simulation, we observe a very wide ($\gtrsim 10^4\,\mathrm{au}$) binary stellar system consisting of $60$ and $70\,M_\odot$ stars. One of the member stars also has two smaller mass ($10\,M_\odot$) companion stars orbiting at $200$ and $800\,\mathrm{au}$, making up a mini-triplet system. Our results suggest that massive binary or multiple systems are common among Pop III stars.