TY - JOUR
T1 - Accretion shocks in a close binary system
AU - Sawada, Keisuke
AU - Matsuda, Takuya
AU - Hachisu, Izumi
N1 - Funding Information:
The authors thank Professor T. Sakurai of Kyoto University for his encouragement. We are also grateful to Mr E. Shima of Kawasaki Heavy Industries for his contribution to developing the numerical code. The computations were performed by the Fujitsu VP100 vector processor at the Data Processing Center of Kyoto University. This work was supported by the Grant-in-Aid for Scientific Research (59540155) of the Ministry of Education and Culture in Japan.
Publisher Copyright:
© Royal Astronomical Society • Provided by the NASA Astrophysics Data System
PY - 1986/8
Y1 - 1986/8
N2 - Numerical simulations of gas flow in a semi-detached close binary system with mass-ratio unity are performed by solving the two-dimensional Euler equation. A star filling its own critical Roche lobe loses mass, while the other compact star accretes it. Two types of flow, i.e. a Roche lobe overflow and a stellar wind, are found to exist. The parameter deciding which type of flow is realized is the sound speed of gas at the surface of the mass-losing star. If the sound speed of the gas is less than A Ω, where A is the separation of the two stars and Ω is the rotational angular frequency of the system, Roche lobe overflow is realized and an accretion disc around the compact star is formed. Two spiral-shaped shock waves are formed on the accretion disc. If the sound speed is larger than A Ω, a stellar wind type of flow is formed. A conical shock originating at the compact star is observed. The transition of these two types of flow is investigated.
AB - Numerical simulations of gas flow in a semi-detached close binary system with mass-ratio unity are performed by solving the two-dimensional Euler equation. A star filling its own critical Roche lobe loses mass, while the other compact star accretes it. Two types of flow, i.e. a Roche lobe overflow and a stellar wind, are found to exist. The parameter deciding which type of flow is realized is the sound speed of gas at the surface of the mass-losing star. If the sound speed of the gas is less than A Ω, where A is the separation of the two stars and Ω is the rotational angular frequency of the system, Roche lobe overflow is realized and an accretion disc around the compact star is formed. Two spiral-shaped shock waves are formed on the accretion disc. If the sound speed is larger than A Ω, a stellar wind type of flow is formed. A conical shock originating at the compact star is observed. The transition of these two types of flow is investigated.
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U2 - 10.1093/mnras/221.3.679
DO - 10.1093/mnras/221.3.679
M3 - Article
AN - SCOPUS:85084299603
SN - 0035-8711
VL - 221
SP - 679
EP - 686
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 3
ER -