TY - JOUR
T1 - The Birth of a Massive First-star Binary
AU - Sugimura, Kazuyuki
AU - Matsumoto, Tomoaki
AU - Hosokawa, Takashi
AU - Hirano, Shingo
AU - Omukai, Kazuyuki
N1 - Funding Information:
2020-03-20 2020-03-26 09:58:13 cgi/release: Article released bin/incoming: New from .zip JSPS JSPS Overseas Research Fellowship JSPS JSPS Research Fellowship MEXT/JSPS 17H02863 MEXT/JSPS 17K05394 MEXT/JSPS 18H05436 MEXT/JSPS 18H05437 MEXT/JSPS 16H05996 MEXT/JSPS 19H09134 MEXT/JSPS 18J01296 MEXT/JSPS 17H01102 MEXT/JSPS 17H02869 MEXT/JSPS 17H06360 yes
Publisher Copyright:
© 2020. The American Astronomical Society. All rights reserved..
PY - 2020/3/20
Y1 - 2020/3/20
N2 - We study the formation of massive Population 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 (104 au) binary stellar system consisting of 60 and 70 M o stars. One of the member stars also has two smaller mass (10 M o) companion stars orbiting at 200 and 800 au, making up a mini-triplet system. Our results suggest that massive binary or multiple systems are common among Population III stars.
AB - We study the formation of massive Population 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 (104 au) binary stellar system consisting of 60 and 70 M o stars. One of the member stars also has two smaller mass (10 M o) companion stars orbiting at 200 and 800 au, making up a mini-triplet system. Our results suggest that massive binary or multiple systems are common among Population III stars.
UR - http://www.scopus.com/inward/record.url?scp=85084433943&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85084433943&partnerID=8YFLogxK
U2 - 10.3847/2041-8213/ab7d37
DO - 10.3847/2041-8213/ab7d37
M3 - Article
AN - SCOPUS:85084433943
SN - 2041-8205
VL - 892
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
IS - 1
M1 - L14
ER -