TY - JOUR

T1 - Is the standard accretion disc model invulnerable?

AU - Sawada, Keisuke

AU - Matsuda, Takuya

AU - Inoue, Minoru

AU - Hachisu, Izumi

N1 - Funding Information:
T. Matsuda would like to acknowledge Professor F. Meyer, Professor M. Takeuchi, Dr H. Ando and Dr T. Hanawa for valuable discussions. He would also like to thank Dr S. Falle for his useful comments and Dr H. C. Spruit for sending his preprint. The computations were performed using the Fujitsu (FACOM) VP200 vector processor at the data processing centre of Kyoto University. This work was supported by a Grant-in-Aid for Scientific Research (59540155) of the Ministry of Education and Culture, Japan.
Publisher Copyright:
© Royal Astronomical Society • Provided by the NASA Astrophysics Data System

PY - 1987

Y1 - 1987

N2 - Two-dimensional hydrodynamic calculations of a gas flow in a semi-detached close binary system with mass ratio unity are carried out again, using a different coordinate system from our previous work (Sawada, Matsuda & Hachisu).The Euler equation is solved using the second-order Osher scheme in a multi-box type of grid, which gives a high resolution about a mass-accreting compact object. Spiral-shaped shock waves in the accretion disc are found to extend down to r=0.01 A, where r and A are the radial distance from the compact star and the separation of two stars respectively. It means that the tidal effect by the mass-losing star is important even so close to the compact object. It is also confirmed that the gas particles lose their angular momentum at the shocks and can spiral in without the help of a turbulent viscosity. The fundamental assumptions of the standard accretion disc model, i.e. an axisymmetric thin disc, the important role of the turbulent viscosity etc., are questioned.

AB - Two-dimensional hydrodynamic calculations of a gas flow in a semi-detached close binary system with mass ratio unity are carried out again, using a different coordinate system from our previous work (Sawada, Matsuda & Hachisu).The Euler equation is solved using the second-order Osher scheme in a multi-box type of grid, which gives a high resolution about a mass-accreting compact object. Spiral-shaped shock waves in the accretion disc are found to extend down to r=0.01 A, where r and A are the radial distance from the compact star and the separation of two stars respectively. It means that the tidal effect by the mass-losing star is important even so close to the compact object. It is also confirmed that the gas particles lose their angular momentum at the shocks and can spiral in without the help of a turbulent viscosity. The fundamental assumptions of the standard accretion disc model, i.e. an axisymmetric thin disc, the important role of the turbulent viscosity etc., are questioned.

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U2 - 10.1093/mnras/224.2.307

DO - 10.1093/mnras/224.2.307

M3 - Article

AN - SCOPUS:0001477568

VL - 224

SP - 307

EP - 322

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 2

ER -